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469705 ǂKá̦gára
469705 ǂKá̦gára (provisional designation 2005 EF298) is a trans-Neptunian object and binary system of the core Kuiper belt, located in the outermost region of the Solar System. It was discovered on 11 March 2005 by American astronomer Marc Buie at the Kitt Peak Observatory in Arizona. [1] The primary body measures around 140 kilometers (90 miles) in diameter. Its 120-kilometer (75-mile) companion ǃHãunu was discovered with the Hubble Space Telescope in 2009. The ǂKá̦gára–ǃHãunu system is currently undergoing mutual occultation and eclipsing events in which one body casts a shadow on or obstructs the view of the other as seen from Earth.
469705 ǂKá̦gára
Stacked Hubble Space Telescope images of ǂKá̦gára and ǃHãunu
Discovery[1]
Discovered byMarc Buie
Discovery siteKitt Peak Observatory
Discovery date11 March 2005
Designations
MPC designation
(469705) ǂKá̦gára
Pronunciation
• English: /ˈkɑːʔɡɑːrə/
• ǀXam: [ǂ͡káˤɡáɾa]
Named after
ǂKá̦gára (San mythology)[2]
Alternative designations
2005 EF298
Minor planet category
Cold classical KBO[2]
Orbital characteristics[3][1]
Epoch (JD 2458600.5)
Uncertainty parameter 3
Observation arc10.10 yr (3688 d)
Aphelion44.058 AU
Perihelion40.013 AU
Semi-major axis
44.081 AU
Eccentricity0.085
Orbital period (sidereal)
292.45 yr (106744.25 d)
Mean anomaly
118.059°
Mean motion
0.00337 0° 0m 0s / day
Inclination1.60°
Longitude of ascending node
118.059°
Argument of perihelion
77.966°
Known satellites1[4]
Physical characteristics
Mean diameter
138+21
−25 km, assuming same albedo as ǃHãunu
Mass(1.29±0.07)×1018 kg, assuming same density and albedo as ǃHãunu
Mean density
1.1+0.9
−0.4 g/cm3, assuming equal compositions of the bodies
Absolute magnitude (H)
HV = 6.2±0.5
Names
The names ǂKá̦gára and ǃHãunu are from the mythology of the ǀXam people of South Africa. ǂKá̦gára (also rendered ǂKaʻgara) and his brother-in-law ǃHãunu fought an epic battle in the east using thunder and lightning, producing mountainous clouds and rain. The conflict was fought over ǂKá̦gára's returning his younger sister, ǃHãunu's wife, to their parents. [2][5] The names were approved and an official naming citation was published on 16 June 2021 by the International Astronomical Union's Working Group on Small Body Nomenclature. [6]
In the ǀXam language, ǂKá̦gára and ǃHãunu are thought to have been pronounced [ǂ͡káˤɡáɾa] [Note 1] and [ᵑ̊ǃʰəunu] ,[Note 2] respectively. [7] The initial letters ǂK and !H (and indeed the letter ǀX in 'ǀXam') represent some of the many click consonants that characterize ǀXam and other San languages. The diacritic under the first vowel in ǂKá̦gára indicates that it is a pharyngealized vowel, another characteristic of San languages. When pronounced in English, the click consonants in words from ǀXam and other San languages are usually ignored (much as Xhosa is pronounced /ˈkoʊzə/ (KOH-zə) rather than [ǁʰosa]), resulting in /ˈkɑːʔɡɑːrə/ (KAHʼ-gar-ə) and /ˈhaʊnuː/ (HOW-noo). ASCII approximations of the names are =Ka'gara and !Haunu.
Orbit and occultations
ǂKá̦gára is a cold classical Kuiper belt object. It orbits the Sun at a distance of 44 AU once every 290 years. Its orbit has an eccentricity of 0.09 and an inclination of 3 degrees with respect to the ecliptic. [3]
If the two bodies are spheres with equal density, then mutual occultation events between ǂKá̦gára and its satellite ǃHãunu should have begun in 2015 and should continue until 2035. When ǂKá̦gára passes in front of ǃHãunu, events may last as long as 8 hours, but when ǃHãunu passes in front of ǂKá̦gára they are expected to last as long as 2 days. These latter events are only expected to occur from 2022 to 2027. [2]
Formation
Prograde orbits dominate tight binary systems such as 469705 ǂKá̦gára, those with satellite semimajor axes less than about 5% of their Hill radii. Grundy et al. suggest that this could be "the signature of planetesimal formation through gravitational collapse of local density enhancements such as caused by the streaming instability",[2] which has been suggested as the formative mechanism of the only visited planetesimal, 486958 Arrokoth.
Satellite, size and mass
ǃHãunu
Discovery
Discovery date2009
Designations
Pronunciation
• English: /ˈhaʊnuː/
• ǀXam: [ᵑ̊ǃʰəunu]
Named after
ǃHãunu (San mythology)[2]
Alternative names
• ǂKá̦gára I
• S/2009 (469705) 1
Orbital characteristics[2][8][4]
Semi-major axis
7670±140 km
Eccentricity0.694±0.013
Orbital period (sidereal)
128.107±0.027 d (prograde)
Inclination
• 33.33°±0.41° ref'd to J2000 equatorial frame
• 11.17°±0.41° to heliocentric orbit
Physical characteristics
Mean diameter
122+16
−19 km , assuming same albedo as ǂKá̦gára
Mass(0.89±0.05)×1018 kg, assuming same density and albedo as ǂKá̦gára
Apparent magnitude
ΔH = 0.59
469705 ǂKá̦gára has one known satellite, ǃHãunu. The magnitude difference between ǂKá̦gára and ǃHãunu is 0.59 mag. This corresponds to a difference in diameter of 13%, if the two bodies have the same albedo. [2]
The system mass is (2.18±0.12)×1018 kg, and, given the albedo, the bodies are equivalent to a single sphere of diameter 174+27
−32 km . This corresponds to a density of 1.1+0.9
−0.4 g/cm3 . This does not particularly constrain the composition of the bodies, as the error bars cover the densities of both small, porous bodies and larger, collapsed bodies. Assuming the two bodies have the same albedo and density, their masses are (1.29±0.07)×1018 kg and (0.89±0.05)×1018 kg, and their diameters are 138+21
−25 km and 122+16
−19 km . [2]
Notes
1. Bleek & Lloyd wrote ⟨ǂk⟩ when the posterior release of the click was audible. | 0 | 0 |
Based on the sounds attested in the closely related language Nǁng, this [ǂ͡k] may therefore represent a palatal pulmonic-contour click, though this is not certain.
2. Based on the co-occurrence of the letter ⟨H⟩ for aspiration of the click and the tilde for nasalization on the following vowel, together with the patterns of sounds in Nǁng, it is suspected that the click in ǃHãunu has delayed aspiration (i.e., is a long, aspirated, nasalized click), rather than a simple IPA: [ǃʰə̃unu], though again this is not certain.
References
1. "469705 (2005 EF298)". Minor Planet Center. Retrieved 7 April 2019.
2. Grundy, W.M. ; Noll, K.S. ; Roe, H.G. ; Buie, M.W. ; Porter, S.B. ; Parker, A.H.; Nesvorný, D.; Levison, H.F.; Benecchi, S.D. ; Stephens, D.C.; Trujillo, C.A. (April 2019). "Mutual orbit orientations of transneptunian binaries". Icarus. 334: 62–78. doi:10.1016/j.icarus.2019.03.035. Retrieved 6 April 2019. (heliocentric parameters averaged over 10Myr)
3. "JPL Small-Body Database Browser: 469705 (2005 EF298)" (2015-04-06 last obs.). Jet Propulsion Laboratory. Retrieved 7 April 2019.
4. Johnston, Wm. Robert (27 May 2019). "Asteroids with Satellites Database – (469705) 2005 EF298". Johnston's Archive. Retrieved 18 June 2021.
5. ≠kagara's fight with !haunu in the east. Lucy Lloyd |xam notebooks, vol. VIII-30, July 1879.
6. "WGSBN Bulletin" (PDF), Working Group Small Body Nomenclature, vol. 1, no. 3, p. 15, 16 June 2021
7. Will Grundy: 469705 (how to say)
8. "ǂKá̦gára and ǃHãunu (469705 2005 EF298)". Mutual Orbits of Binary Transneptunian Objects. Retrieved 7 April 2019. (heliocentric parameters averaged over 10Myr)
External links
• Asteroids with Satellites, Johnston's Archive
• List of Known Trans-Neptunian Objects, Johnston's Archive
• List of Transneptunian Objects, Minor Planet Center
• 469705 ǂKá̦gára at the JPL Small-Body Database
• 469705 ǂKá̦gára at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
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• 469705 ǂKá̦gára
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(111253) 2001 XU10
(111253) 2001 XU10 (provisional designation 2001 XU10) is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers in diameter. It was discovered on 9 December 2001, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [2] The asteroid is one of the largest potentially hazardous asteroids. [4]
(111253) 2001 XU10
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date9 December 2001
Designations
MPC designation
(111253) 2001 XU10
Alternative designations
2001 XU10
Minor planet category
Apollo · NEO · PHA[1][2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc17.94 yr (6,552 days)
Aphelion2.5242 AU
Perihelion0.9832 AU
Semi-major axis
1.7537 AU
Eccentricity0.4394
Orbital period (sidereal)
2.32 yr (848 days)
Mean anomaly
38.733°
Mean motion
0° 25m 27.84s / day
Inclination42.020°
Longitude of ascending node
310.17°
Argument of perihelion
6.9341°
Earth MOID0.0293 AU · 11.4 LD
Physical characteristics
Dimensions3.006±0.893 km[3]
Geometric albedo
0.178±0.156[3]
Absolute magnitude (H)
15.2[1]
Orbit and classification
2001 XU10 orbits the Sun at a distance of 0.98–2.52 AU once every 2 years and 4 months (848 days; semi-major axis of 1.75 AU). Its orbit has an eccentricity of 0.44 and an inclination of 42° with respect to the ecliptic. [1] The body's observation arc begins with a precovery taken by the Sloan Digital Sky Survey in February 2000. [2]
2001 XU10 is a member of the Apollo asteroids, the largest subgroup of near-Earth asteroids which cross the orbit of Earth. It is also a Mars-crosser, as it crosses the orbit of the Red Planet at 1.66 AU. [1]
Close approaches
With an absolute magnitude of 15.2, 2001 XU10 is one of the brightest and presumably largest known potentially hazardous asteroid. [4] It has an Earth minimum orbital intersection distance of 0.0293 AU (4,380,000 km), which translates into 11.4 lunar distances (LD). [1] On 29 July 2054, this asteroid will make its closest near-Earth encounter of the 21st century at a nominal distance of 0.079 AU (31.1 LD). [1]
Physical characteristics
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2001 XU10 measures 3.006 kilometers in diameter and its surface has an albedo of 0.178. [3]
As of 2018, no rotational lightcurve of 2001 XU10 has been obtained from photometric observations. The asteroid's rotation period, spin axis and shape remain unknown. In addition, the body's spectral type has never been assessed. [1][5]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 19 October 2005. [6] As of 2018, it has not been named. [2]
References
1. "JPL Small-Body Database Browser: 111253 (2001 XU10)" (2018-01-16 last obs.). Jet Propulsion Laboratory. Retrieved 19 January 2018.
2. "111253 (2001 XU10)". Minor Planet Center. Retrieved 19 January 2018.
3. Mainzer, A.; Grav, T.; Masiero, J.; Bauer, J.; Cutri, R. M.; McMillan, R. S.; et al. (November 2012). "Physical Parameters of Asteroids Estimated from the WISE 3-Band Data and NEOWISE Post-Cryogenic Survey". The Astrophysical Journal Letters. 760 (1): 6. arXiv:1210.0502. Bibcode:2012ApJ...760L..12M. doi:10.1088/2041-8205/760/1/L12.
4. "List of the Potentially Hazardous Asteroids (PHAs)". Minor Planet Center. Retrieved 19 January 2018.
5. "LCDB Data for (111253)". Asteroid Lightcurve Database (LCDB). Retrieved 19 January 2018.
6. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• (111253) 2001 XU10 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (111253) 2001 XU10 at ESA–space situational awareness
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• (111253) 2001 XU10 at the JPL Small-Body Database
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11351 Leucus
11351 Leucus /ˈljuːkəs/ is a mid-sized Jupiter trojan from the Greek camp, approximately 40 kilometers (25 miles) in diameter. It is a target of the Lucy mission, scheduled for a flyby in April 2028. [8][10] The assumed D-type asteroid is an exceptionally slow rotator with a rotation period of 466 hours. [3] It was discovered on 12 October 1997 by the Beijing Schmidt CCD Asteroid Program (SCAP) at Xinglong Station in the Chinese province of Hebei, and later named after the Achaean warrior Leucus from Greek mythology. [1]
11351 Leucus
Shape model of Leucus viewed from multiple orthogonal perspectives
Discovery[1]
Discovered bySCAP
Discovery siteBeijing Xinglong Obs.
Discovery date12 October 1997
Designations
MPC designation
(11351) Leucus
Pronunciation/ˈljuːkəs/[2]
Named after
Leucus (Greek mythology)[1]
Alternative designations
1997 TS25 · 1996 VP39
Minor planet category
Jupiter trojan[1][3]
Greek[4] · background[5]
Orbital characteristics[3]
Epoch 25 February 2023 (JD 2460000.5)
Uncertainty parameter 0
Earliest precovery date25 July 1982[1]
Aphelion5.652 AU
Perihelion4.953 AU
Semi-major axis
5.302 AU
Eccentricity0.0659
Orbital period (sidereal)
12.21 yr (4,460 d)
Mean anomaly
43.784°
Mean motion
0° 4m 50.607s / day
Inclination11.546°
Longitude of ascending node
251.087°
Argument of perihelion
160.955°
Jupiter MOID0.0942 AU
TJupiter2.955
Physical characteristics
Dimensions63.8 × 36.6 × 29.6 km[6]
Mean diameter
41 km (volume equivalent)[6]
Synodic rotation period
445.683±0.007 h[7][3]
Axial tilt
13° (wrt ecliptic)[7]
10° (wrt orbit)[7]
Pole ecliptic latitude
+77°[7]
Pole ecliptic longitude
208°[7]
Geometric albedo
0.037±0.001[6]
Spectral type
D[8]
B–V = 0.739±0.044[9]
V–R = 0.498±0.044[9]
V–I = 0.900±0.057[9]
Absolute magnitude (H)
10.979±0.037[7]
Orbit and classification
Leucus is a dark Jupiter trojan asteroid in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at Jupiter's L4 Lagrangian point, 60° ahead of its orbit (see Trojans in astronomy). It is also a non-family asteroid in the Jovian background population. [5]
It orbits the Sun at a distance of 5.0–5.6 AU once every 12 years and 2 months (4,440 days; semi-major axis of 5.29 AU). Its orbit has an eccentricity of 0.06 and an inclination of 12° with respect to the ecliptic. [3] The body's observation arc begins with a precovery taken at the Siding Spring Observatory in July 1982, more than 15 years prior to its official discovery observation at Xinglong. [1]
Exploration
Lucy mission target
Leucus is planned to be visited by the Lucy spacecraft, which launched in 2021. The flyby is scheduled for 18 April 2028, and will approach the asteroid to a distance of 1,000 km (620 mi) at a relative velocity of 5.9 km/s (13,000 mph). [8]
Physical characteristics
Leucus is a D-type asteroid,[8] which is the dominant spectral type among the Jupiter trojans, with the remainder being mostly carbonaceous C-type and primitive P-type asteroids.
Slow rotator
During spring 2013, a rotational lightcurve of Leucus was obtained from photometric observations made by astronomers Robert Stephens and Daniel Coley at the Center for Solar System Studies (CS3), California, using a 0.35/0.4-meter Schmidt-Cassegrain telescope. The lightcurve showed an exceptionally slow rotation period of 513.7 hours with a brightness variation of 0.53 in magnitude (U=2+). No evidence of a non-principal axis rotation (NPAR) was found. [11] It is one of the slowest rotators known to exist.
In preparation for the planned visit by the Lucy spacecraft, Leucus was once again observed by astronomers Marc Buie at SwRI and Stefano Mottola at DLR in 2016. The obtained bimodal lightcurve gave a somewhat shorter period of 440 hours and an amplitude of 0.7 magnitude. [12]
Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Leucus has a low albedo of 0.06 and 0.08, with a diameter of 42.1 and 34.2 kilometers, respectively. [13][14] The Collaborative Asteroid Lightcurve Link derives a lower albedo of 0.05 and a diameter of 42.1 kilometers, in accordance with the result obtained by IRAS. [15]
Naming
This minor planet was named from Greek mythology, after the Achaean warrior Leucus in Homer's Iliad. He was a companion of Odysseus. [1] Leucus was killed during the Trojan War by Antiphus, one of the fifty sons of King Priam of Troy. [16] The approved naming citation was published by the Minor Planet Center on 22 February 2016 (M.P.C. 98711). [17]
References
1. "11351 Leucus (1997 TS25)". Minor Planet Center. Retrieved 22 June 2018.
2. Noah Webster (1884) A Practical Dictionary of the English Language
3. "JPL Small-Body Database Browser: 11351 Leucus (1997 TS25)" (2017-06-07 last obs.). Jet Propulsion Laboratory. Retrieved 22 June 2018.
4. "List of Jupiter Trojans". Minor Planet Center. 1 June 2018. Retrieved 22 June 2018.
5. "Asteroid (11351) Leucus – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 22 June 2018.
6. Buie, Marc W.; Keeney, Brian A.; Strauss, Ryder A.; Blank, Ted E.; Moore, John G.; Porter, Simon B. (October 2021). "Size and Shape of (11351) Leucus from Five Occultations". The Planetary Science Journal. 2 (5): 38. Bibcode:2021PSJ.....2..202B. doi:10.3847/PSJ/ac1f9b. S2CID 237623594. 202.
7. Mottola, Stefano; Hellmich, Stephan; Buie, Marc W.; Zangari, Amanda M.; Marchi, Simone; Brown, Michael E.; Levison, Harold F. (December 2020). "Convex Shape and Rotation Model of Lucy Target (11351) Leucus from Lightcurves and Occultations". The Planetary Science Journal. 1 (3): 14. arXiv:2009.08951. Bibcode:2020PSJ.....1...73M. doi:10.3847/PSJ/abb942. S2CID 221802440. 73.
8. Levison, H. F.; Olkin, C.; Noll, K. S.; Marchi, S.; Lucy Team (March 2017). "Lucy: Surveying the Diversity of the Trojan Asteroids: The Fossils of Planet Formation" (PDF). 48th Lunar and Planetary Science Conference (1964): 2025. Bibcode:2017LPI....48.2025L. Retrieved 13 April 2017.
9. Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited". Astronomy and Astrophysics. 546: 20. arXiv:1209.1896. Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. | 2 | 0 |
S2CID 54776793.
10. Casey Dreier; Emily Lakdawalla (30 September 2015). "NASA announces five Discovery proposals selected for further study". The Planetary Society. Retrieved 12 April 2017.
11. French, Linda M.; Stephens, Robert, D.; Coley, Daniel R.; Wasserman, Lawrence H.; Vilas, Faith; La Rocca, Daniel (October 2013). "A Troop of Trojans: Photometry of 24 Jovian Trojan Asteroids". The Minor Planet Bulletin. 40 (4): 198–203. Bibcode:2013MPBu...40..198F. ISSN 1052-8091. {{cite journal}}: CS1 maint: multiple names: authors list (link)
12. Buie, Marc W.; Zangari, Amanda Marie; Marchi, Simone; Mottola, Stefano; Levison, Harold F. (October 2016). "Ground-based characterization of Leucus and Polymele, two fly-by targets of the Lucy Discovery mission". American Astronomical Society. 48: 208.06. Bibcode:2016DPS....4820806B.
13. Grav, T.; Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.; Nugent, C. R. (November 2012). "WISE/NEOWISE Observations of the Jovian Trojan Population: Taxonomy". The Astrophysical Journal. 759 (1): 10. arXiv:1209.1549. Bibcode:2012ApJ...759...49G. doi:10.1088/0004-637X/759/1/49. S2CID 119101711. (online catalog)
14. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System – IRAS-A-FPA-3-RDR-IMPS-V6.0: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 15 June 2018.
15. "LCDB Data for (11351) Leucus". Asteroid Lightcurve Database (LCDB). Retrieved 22 June 2018.
16. Homer, Iliad, 4. 491
17. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 22 June 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Discovery Circumstances: Numbered Minor Planets (10001)-(15000) – Minor Planet Center
• Asteroid 11351 Leucus at the Small Bodies Data Ferret
• 11351 Leucus at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 11351 Leucus at the JPL Small-Body Database
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• 11350 Teresa
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• 11352 Koldewey
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(11474) 1982 SM2
(11474) 1982 SM2 is a carbonaceous Baptistina asteroid and potentially slow rotator from the inner regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 18 September 1982, by Belgian astronomer Henri Debehogne at ESO' La Silla Observatory in northern Chile. [5]
(11474) 1982 SM2
Discovery[1]
Discovered byH. Debehogne
Discovery siteLa Silla Obs.
Discovery date18 September 1982
Designations
MPC designation
(11474) 1982 SM2
Alternative designations
1982 SM2 · 1995 KD
Minor planet category
main-belt · Baptistina[2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc32.59 yr (11,905 days)
Aphelion2.7224 AU
Perihelion1.8294 AU
Semi-major axis
2.2759 AU
Eccentricity0.1962
Orbital period (sidereal)
3.43 yr (1,254 days)
Mean anomaly
76.029°
Mean motion
0° 17m 13.56s / day
Inclination5.4069°
Longitude of ascending node
348.59°
Argument of perihelion
355.61°
Physical characteristics
Dimensions5.71 km (calculated)[2]
Synodic rotation period
1917.2214±2716 h[3]
Geometric albedo
0.057 (assumed)[2]
Spectral type
C[2]
Absolute magnitude (H)
14.493±0.001 (R)[3] · 14.7[1] · 14.94[2] · 14.94±0.61[4]
Orbit and classification
The C-type asteroid belongs to the small Baptistina family. It orbits the Sun at a distance of 1.8–2.7 AU once every 3 years and 5 months (1,254 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. [1] As no precoveries were taken, and no prior identifications were made, the asteroid's observation arc begins with its official discovery observation. [5]
Physical characteristics
In September 2013, a rotational lightcurve of this asteroid was obtained from photometric observations in the R-band at the Palomar Transient Factory in California. It gave an exceptionally long rotation period of 1917 hours with a brightness amplitude of 0.04 magnitude (U=1). [3] However, the fragmentary light-curve has received a low quality rating by the Collaborative Asteroid Lightcurve Link (CALL) which means that the result could be completely wrong (also see potentially slow rotator). [2][3]
CALL assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 5.71 kilometers, based on an absolute magnitude of 14.49. [2]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 28 September 1999. [6] As of 2018, it has not been named. [5]
References
1. "JPL Small-Body Database Browser: 11474 (1982 SM2)" (2015-04-23 last obs.). Jet Propulsion Laboratory. Retrieved 26 May 2017.
2. "LCDB Data for (11474)". Asteroid Lightcurve Database (LCDB). Retrieved 16 December 2016.
3. Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. S2CID 8342929. Retrieved 16 December 2016.
4. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339. Retrieved 16 December 2016.
5. "11474 (1982 SM2)". Minor Planet Center. Retrieved 16 December 2016.
6. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• Discovery Circumstances: Numbered Minor Planets (10001)-(15000) – Minor Planet Center
• (11474) 1982 SM2 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (11474) 1982 SM2 at the JPL Small-Body Database
Minor planets navigator
• 11473 Barbaresco
• (11474) 1982 SM2
• 11475 Velinský
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(118228) 1996 TQ66
(118228) 1996 TQ66 (provisional designation 1996 TQ66) is a resonant trans-Neptunian object of the plutino population in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 October 1996, by American astronomers Jun Chen, David Jewitt, Chad Trujillo, and Jane Luu, using the UH88 telescope at the Mauna Kea Observatories, Hawaii. [1][2] The very red object measures approximately 185 kilometers (110 miles) in diameter. As of 2021, it has not been named.
(118228) 1996 TQ66
Discovery[1][2]
Discovered byJ. Chen
D. C. Jewitt
C. Trujillo
J. X. Luu
Discovery siteMauna Kea Obs.
Discovery date8 October 1996
Designations
MPC designation
(118228) 1996 TQ66
Alternative designations
1996 TQ66
Minor planet category
TNO[3] · plutino[4][5]
Orbital characteristics[3]
Epoch 1 July 2021 (JD 2459396.5)
Uncertainty parameter 2
Observation arc24.17 yr (8,828 d)
Aphelion44.219 AU
Perihelion34.535 AU
Semi-major axis
39.377 AU
Eccentricity0.1230
Orbital period (sidereal)
247.10 yr (90,254 d)
Mean anomaly
33.659°
Mean motion
0° 0m 14.4s / day
Inclination14.650°
Longitude of ascending node
10.613°
Argument of perihelion
18.541°
Physical characteristics
Mean diameter
185 km (est. at 0.09)[4]
Spectral type
• RR (very red)[6][7]
• B–V = 1.190±0.020[6]
• V–R = 0.660±0.030[6]
• V–I = 1.440±0.140[6]
Apparent magnitude
22.85[8]
Absolute magnitude (H)
7.14[2][3]
Orbit and classification
1996 TQ66 orbits the Sun at a distance of 34.5–44.2 AU once every 247 years and 1 month (90,254 days; semi-major axis of 39.38 AU). Its orbit has an eccentricity of 0.12 and an inclination of 15° with respect to the ecliptic. [3] The body's observation arc begins with its official discovery observation at the Mauna Kea Observatories on 8 October 1996. [2] It came to perihelion in 1998. As of 2021, it is at 35.6 AU from the Sun and has an apparent magnitude of 22.85. [8]
1996 TQ66 is a trans-Neptunian object and belongs to the plutino population,[4][5] a large group of objects named after their largest member, Pluto. These resonant trans-Neptunian objects stay in a 2:3 mean-motion orbital resonance with Neptune, orbiting exactly two times the Sun for every three orbits Neptune does and are therefore protected from Neptune's scattering effect. Plutinos are located in the inner rim of the Kuiper belt, a large circumstellar disc of mostly non-resonant classical Kuiper belt objects.
Numbering and naming
1996 TQ66 was numbered by the Minor Planet Center on 16 November 2005, receiving the number (118228) in the minor planet catalog (M.P.C. 55524). [9] As of 2021, it has not been named. [2] According to the established naming conventions, it will be given a mythological name associated with the underworld. [10]
Physical characteristics
1996 TQ66 has a very red surface color (RR) in the visible part of the spectrum, with B−V and V–R color indices of 1.190±0.020 and 0.660±0.030, respectively, for a combined B−R magnitude of 1.85. [4][6][7] A red surface color is typically associated with the presence of tholins, polymer-like organic compounds, formed by long exposures to solar and cosmic radiation.
Rotation period
In 1999, results of a photometric survey of Kuiper belt objects by Romanishin and Tegler were published in the Journal Nature. For 1996 TQ66, a brightness variation of no more than 0.22 in magnitude could be determined, which is indicative of a modestly irregular shape. [7][11] As of 2021, no rotational lightcurve for this object has been obtained from photometry. The body's rotation period, pole and actual shape remain unknown. [3][7]
Diameter and albedo
Based on a generic magnitude-to-diameter conversion, 1996 TQ66 measures approximately 185 kilometers (110 miles) in diameter, for an assumed albedo of 0.9 and an magnitude of 7. [4][12] According to Mike Brown, who estimates a mean-diameter of 186 km (120 mi), the object is too small for being considered a dwarf planet candidate ("probably not"). [13]
References
1. "MPEC 1997-N09 : 1996 TQ66". Minor Planet Electronic Circular. Minor Planet Center. 7 July 1997. Retrieved 9 September 2021.
2. "118228 (1996 TQ66)". Minor Planet Center. Retrieved 10 September 2021.
3. "JPL Small-Body Database Browser: 118228 (1996 TQ66)" (2020-12-09 last obs.). Jet Propulsion Laboratory. Retrieved 10 September 2021.
4. "List of Known Trans-Neptunian Objects". Johnston's Archive. 18 August 2020. Retrieved 10 September 2021.
5. "Orbit Fit and Astrometric record for 118228". Southwest Research Institute. Retrieved 10 September 2021.
6. Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Dovgopol, Anatolij N. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus. 250: 482–491. Bibcode:2015Icar..250..482B. doi:10.1016/j.icarus.2014.12.004. ISSN 0019-1035.
7. "LCDB Data for (118228)". Asteroid Lightcurve Database (LCDB). Retrieved 10 September 2021.
8. "Asteroid (118228) 1996 TQ66 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site. Retrieved 10 September 2021.
9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 10 September 2021.
10. "Naming of Astronomical Objects – Minor planets". IAU – International Astronomical Union. Retrieved 27 July 2021.
11. Romanishin, W.; Tegler, S. C. (March 1999). "Rotation rates of Kuiper-belt objects from their light curves". Nature. 398 (6723): 129–132. Bibcode:1999Natur.398..129R. doi:10.1038/18168. ISSN 0028-0836. S2CID 4313184.
12. "Asteroid Size Estimator". CNEOS NASA/JPL. Retrieved 10 September 2021.
13. Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 10 September 2021.
External links
• MPEC 1997-N20 : 1996 TQ66, Minor Planet Electronic Circular
• (118228) 1996 TQ66, Small Bodies Data Ferret
• Kuiper Belt Object Magnitudes and Surface Colors, Stephen C. Tegler (archived)
• List of Transneptunian Objects, Minor Planet Center
• Discovery Circumstances: Numbered Minor Planets (115001)–(120000), Minor Planet Center
• (118228) 1996 TQ66 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (118228) 1996 TQ66 at the JPL Small-Body Database
Trans-Neptunian objects
TNO classes | 4 | 0 |
• Cubewanos
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• Vanth
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• Haumea
• Namaka
• Hiʻiaka
• Ring
• Quaoar
• Weywot
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• Makemake
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• Gonggong
• Xiangliu
• Eris
• Dysnomia
• Sedna
Sednoids
• 90377 Sedna
• 2012 VP113
• 541132 Leleākūhonua
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• (118228) 1996 TQ 66
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(118378) 1999 HT11
(118378) 1999 HT11 (provisional designation 1999 HT11) is a trans-Neptunian object from the outermost region of the Solar System, locked in a 4:7 orbital resonance with Neptune. It was discovered on 17 April 1999, by astronomers at the Kitt Peak Observatory, Arizona, in the United States. [2] The very red object measures approximately 134 kilometers (83 miles) in diameter. As of 2021, it has not been named.
(118378) 1999 HT11
Discovery[1][2]
Discovered byKitt Peak National Obs.
Discovery siteKitt Peak National Obs.
Discovery date17 April 1999
Designations
MPC designation
(118378) 1999 HT11
Alternative designations
1999 HT11
Minor planet category
TNO[3] · res (4:7)[4][5]
Orbital characteristics[3]
Epoch 1 July 2021 (JD 2459396.5)
Uncertainty parameter 3[2][3]
Observation arc20.78 yr (7,589 d)
Aphelion49.001 AU
Perihelion38.734 AU
Semi-major axis
43.868 AU
Eccentricity0.1170
Orbital period (sidereal)
290.55 yr (106,124 d)
Mean anomaly
328.33°
Mean motion
0° 0m 12.24s / day
Inclination5.0489°
Longitude of ascending node
87.954°
Argument of perihelion
189.27°
Physical characteristics
Mean diameter
134 km (est. at 0.09)[4]
Spectral type
• RR (very red)[4]
• B–V = 1.150±0.064[6][7]
• V–R = 0.670±0.040[6][7]
• B–R = 1.820±0.050[6][7]
Apparent magnitude
23.42[8]
Absolute magnitude (H)
7.6[2][3]
Discovery
1999 HT11 was first observed on the night of 17 April 1999, by astronomers using the 4-meter Nicholas U. Mayall Telescope at Kitt Peak National Observatory in Arizona. Five additional objects were discovered on the same weekend: 1999 HR11, 1999 HS11, 1999 HU11 (Deucalion), 1999 HV11 and 1999 HW11. The observing astronomers were Robert Millis, James Elliot, Matthew Holman, Mark Wagner as well as Kim Falinski. Follow-up observations with the Nordic Optical Telescope at the Roque de los Muchachos Observatory, La Palma, Spain, were made three weeks later. The body's observation arc begins with its official discovery observation at Kitt Peak on 17 April 1999. [1][2]
Orbit and classification
This minor planet orbits the Sun at a distance of 38.7–49.0 AU once every 290 years and 7 months (106,124 days; semi-major axis of 43.87 AU). Its orbit has an eccentricity of 0.12 and an inclination of 5° with respect to the ecliptic. [3] As of 2021, it is at 39.7 AU from the Sun with an apparent magnitude of 23.42,[8] and will come to perihelion in 2047. [3]
1999 HT11 is a resonant trans-Neptunian object that stays in a 4:7 mean-motion orbital resonance with Neptune, orbiting exactly four times the Sun for every seven orbits Neptune does and are therefore protected from the planets scattering effect. The classification is deemed secure. [4][5] The 4:7 resonance is located in the midst of the classical objects of the Kuiper belt, a circumstellar disc of otherwise non-resonant bodies, contrary to the more prominent resonant plutinos (2:3) and twotinos (1:2) which form the inner and outer rim of the Kuiper belt, respectively.
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 16 November 2005, receiving the number (118378) in the minor planet catalog (M.P.C. 55526). [9] As of 2021, it has not been named. [2] According to the established naming conventions, it will be given a mythological name associated with the underworld or with creation. [10]
Physical characteristics
1999 HT11 has a very red surface color (RR) in the visible part of the spectrum, with B−V and V–R color indices of 1.150±0.064 and 0.670±0.040, respectively, for a combined B−R magnitude of 1.820±0.050. [4][6][7] A red surface color is typically associated with the presence of tholins, polymer-like organic compounds, formed by long exposures to solar and cosmic radiation.
Based on a generic magnitude-to-diameter conversion, 1999 HT11 measures approximately 134 kilometers (83 miles) in diameter, for an assumed albedo of 0.9 and an magnitude of 7.6. [4][11] According to Mike Brown, who estimates a mean-diameter of 137 km (85 mi), the object is too small for being considered a dwarf planet candidate ("probably not"). [12] As of 2021, no rotational lightcurve for this body has been obtained from photometric observations. Its rotation period, pole and shape remain unknown. [3]
References
1. "MPEC 1999-K12 : SIX TNOs (including J99H11T)". Minor Planet Electronic Circular. Minor Planet Center. 19 May 1999. Retrieved 9 September 2021.
2. "118378 (1999 HT11)". Minor Planet Center. Retrieved 11 September 2021.
3. "JPL Small-Body Database Browser: 118378 (1999 HT11)" (2020-01-26 last obs.). Jet Propulsion Laboratory. Retrieved 11 September 2021.
4. "List of Known Trans-Neptunian Objects". Johnston's Archive. 18 August 2020. Retrieved 11 September 2021.
5. "Orbit Fit and Astrometric record for 118378". Southwest Research Institute. Retrieved 11 September 2021. (The Deep Ecliptic Survey Object Classifications)
6. Sheppard, Scott S. (December 2012). "The Color Differences of Kuiper Belt Objects in Resonance with Neptune". The Astronomical Journal. 144 (6): 169. arXiv:1210.0537. Bibcode:2012AJ....144..169S. doi:10.1088/0004-6256/144/6/169. ISSN 0004-6256. S2CID 53746049.
7. "LCDB Data for (118378)". Asteroid Lightcurve Database (LCDB). Retrieved 11 September 2021.
8. "Asteroid (118378) 1999 HT11 – Ephemerides". AstDyS-2, Asteroids – Dynamic Site. Retrieved 11 September 2021.
9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 11 September 2021.
10. "Naming of Astronomical Objects – Minor planets". IAU – International Astronomical Union. Retrieved 11 September 2021.
11. "Asteroid Size Estimator". CNEOS NASA/JPL. Retrieved 11 September 2021.
12. Brown, Michael E. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 11 September 2021.
External links
• List of Transneptunian Objects, Minor Planet Center
• (118378) 1999 HT11, Small Bodies Data Ferret
• Discovery Circumstances: Numbered Minor Planets (115001)-(120000), Minor Planet Center
• (118378) 1999 HT11 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (118378) 1999 HT11 at the JPL Small-Body Database
Trans-Neptunian objects
TNO classes
• Cubewanos
• Scattered-disc objects
• Detached objects
• Resonant objects
• Neptune trojans
• Plutinos
• Twotinos
• TNO moons
Dwarf planets (moons)
• Orcus
• Vanth
• Pluto
• Charon
• Styx
• Nix
• Kerberos
• Hydra
• Haumea
• Namaka | 5 | 0 |
• Hiʻiaka
• Ring
• Quaoar
• Weywot
• Rings
• Makemake
• MK2
• Gonggong
• Xiangliu
• Eris
• Dysnomia
• Sedna
Sednoids
• 90377 Sedna
• 2012 VP113
• 541132 Leleākūhonua
• 2021 RR205
Minor planets navigator
• (118378) 1999 HT 11
• (118379) 1999 HC12
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121 Hermione
Hermione (minor planet designation: 121 Hermione) is a very large binary asteroid discovered in 1872. It orbits in the Cybele group in the far outer asteroid belt. [11] As an asteroid of the dark C spectral type, it is probably composed of carbonaceous materials. In 2002, a small moon was found to be orbiting Hermione. [11]
121 Hermione
121 Hermione and its moon
Discovery[1]
Discovered byJames Craig Watson
Discovery date12 May 1872
Designations
MPC designation
(121) Hermione
Pronunciation/hɜːrˈmaɪ.əniː/[2]
Named after
Hermione[3]
(Greek mythology)
Alternative designations
A872 JA; 1970 VE
Minor planet category
main-belt · Cybele
AdjectivesHermionean /hɜːrmaɪ.əˈniːən/
Orbital characteristics[4]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc145.96 yr (53,312 d)
Aphelion3.9067 AU
Perihelion2.9889 AU
Semi-major axis
3.4478 AU
Eccentricity0.1331
Orbital period (sidereal)
6.40 yr (2,338 d)
Mean anomaly
157.08°
Mean motion
0° 9m 14.4s / day
Inclination7.5975°
Longitude of ascending node
73.127°
Argument of perihelion
298.18°
Known satellitesS/2002 (121) 1
Physical characteristics
Dimensions268 × 186 × 183 km[5]
(254 ± 4) × (125 ± 9) km[6]
Mean radius
95 km[6]
Volume(3.0±0.4)×106 km3[7]
Mass(5.381±5%)×1018 kg[7]
Mean density
1.8 ± 0.2 g/cm3[7][lower-alpha 1]
Equatorial surface gravity
0.022 m/s2[lower-alpha 2]
Equatorial escape velocity
0.075 km/s[lower-alpha 2]
Sidereal rotation period
0.2313 d (5.551 h)[8]
Axial tilt
73°
Pole ecliptic latitude
+10 ± 2°[7]
Pole ecliptic longitude
1.5 ± 2°
Geometric albedo
0.0482 ± 0.002[9]
Spectral type
C[10]
Absolute magnitude (H)
7.31[9]
Discovery
Hermione was discovered by J. C. Watson on 12 May 1872 from Ann Arbor, Michigan, in the United States,[11] and named after Hermione, daughter of Menelaus and Helen in Greek mythology. [3]
Physical properties
The asteroid has a bi-lobed shape, as evidenced by adaptive optics images, the first of which were taken in December 2003 with the Keck telescope. [6] Of several proposed shape models that agreed with the images, a "snowman"-like shape was found to best fit the observed precession rate of Hermione's satellite. [7] In this "snowman" model, the asteroid's shape can be approximated by two partially overlapping spheres of radii 80 and 60 km, whose centers are separated by a distance of 115 km. A simple ellipsoid shape was ruled out.
Observation of the satellite's orbit has made possible an accurate determination of Hermione's mass. [7] For the best-fit "snowman" model, the density is found to be 1.8 ± 0.2 g/cm3, giving a porosity on the order of 20%, and possibly indicating that the main components are fractured solid bodies, rather than the asteroid being a rubble pile.
Occultations by Hermione have been successfully observed three times so far, the last time in February 2004.
S/2002 (121) 1
Discovery[12]
Discovered byW. J. Merline,
P. M. Tamblyn,
C. Dumas,
L. M. Close,
C. R. Chapman,
F. Menard,
W. M. Owen,
and D. C. Slater
Discovery date2002-09-28
Designations
Alternative designations
LaFayette
Minor planet category
main-belt · Cybele
Orbital characteristics[13]
Semi-major axis
768 ± 11 km
Eccentricity0.001 ± 0.001
Orbital period (sidereal)
2.582 ± 0.002 d
Inclination3 ± 2°
(with respect to Hermione pole)
Satellite of121 Hermione
Physical characteristics
Dimensions12 ± 4 km[6]
Mass~1.6×1015 kg[lower-alpha 3]
Absolute magnitude (H)
13.0[6]
Moon
A satellite of Hermione was discovered in 2002 with the Keck II telescope. [11] It is about 8 miles (13 km) in diameter. [11] The satellite is provisionally designated S/2002 (121) 1. It has not yet been officially named, but "LaFayette" has been proposed by a group of astronomers in reference to the frigate used in secret by the Marquis de Lafayette to reach America to help the insurgents. [14][6]
Notes
1. Using the "snowman" shape model, which best matches the value of J2 implied from precession.
2. On the extremities of the long axis.
3. Assuming a similar density to the primary.
References
1. "121 Hermione". Minor Planet Center. Retrieved 14 September 2018.
2. Noah Webster (1884) A Practical Dictionary of the English Language
3. Schmadel, Lutz D. (2007). "(121) Hermione". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 26. doi:10.1007/978-3-540-29925-7_122. ISBN 978-3-540-00238-3.
4. "JPL Small-Body Database Browser: 121 Hermione" (2018-05-25 last obs.). Jet Propulsion Laboratory. Retrieved 14 September 2018.
5. Jim Baer (2008). "Recent Asteroid Mass Determinations". Personal Website. Archived from the original on 2 July 2013. Retrieved 7 December 2008.
6. F. Marchis; et al. (2006). "Shape, size and multiplicity of main-belt asteroids I. Keck Adaptive Optics survey". Icarus. 185 (1): 39–63. Bibcode:2006Icar..185...39M. doi:10.1016/j.icarus.2006.06.001. PMC 2600456. PMID 19081813.
7. F. Marchis; et al. (2005). "Mass and density of Asteroid 121 Hermione from an analysis of its companion orbit". Icarus. 178 (2): 450–464. Bibcode:2005Icar..178..450M. doi:10.1016/j.icarus.2005.05.003.
8. IAUC 8264 Archived 9 July 2008 at the Wayback Machine
9. Supplemental IRAS minor planet survey Archived 2009-08-17 at the Wayback Machine
10. PDS node taxonomy database Archived 2009-08-05 at the Wayback Machine
11. Linda T. Elkins-Tanton (2010). Asteroids, Meteorites, and Comets. Infobase Publishing. p. 96. ISBN 978-1-4381-3186-3.
12. IAUC 7980 Archived 2006-05-01 at the Wayback Machine
13. 121 Hermione and S/2002 (121) 1, orbit data website maintained by F. Marchis.
14. Johnston, Wm. Robert (21 September 2014). "(121) Hermione and S/2002 (121) 1 ("LaFayette")". Asteroids with Satellites Database. Johnston's Archive. Retrieved 7 November 2021.
External links
• 121 Hermione and S/2002 (121) 1, orbit data website maintained by F. Marchis. Includes adaptive optics images, orbit diagrams, and shape models.
• (121) Hermione, datasheet, johnstonsarchive.net
• Asteroids with Satellites, Robert Johnston, johnstonsarchive.net | 6 | 0 |
• Tally of Asteroids Harboring Moons Grows Beyond 30 (Space.com, 3 October 2002)
• 121 Hermione at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 121 Hermione at the JPL Small-Body Database
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(126154) 2001 YH140
(126154) 2001 YH140 (provisional designation 2001 YH140) is a resonant trans-Neptunian object discovered on 18 December 2001, by American astronomers Chad Trujillo and Michael Brown at the Palomar Observatory in California. It measures approximately 345 kilometers in diameter. [4]
(126154) 2001 YH140
Discovery
Discovered byMichael E. Brown,
Chadwick A. Trujillo[1]
Discovery date18 December 2001
Designations
MPC designation
(126154) 2001 YH140
Minor planet category
TNO (3:5 resonance)[2]
Orbital characteristics[1][3]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 2
Observation arc4777 days (13.08 yr)
Aphelion48.725 AU (7.2892 Tm)
Perihelion36.428 AU (5.4496 Tm)
Semi-major axis
42.577 AU (6.3694 Tm)
Eccentricity0.14441
Orbital period (sidereal)
277.82 yr (101475 d)
Mean anomaly
19.455°
Mean motion
0° 0m 12.772s / day
Inclination11.069°
Longitude of ascending node
108.84°
Argument of perihelion
356.62°
Physical characteristics
Dimensions345 ± 45 km[4]
Mass~4.0×1019 kg
Synodic rotation period
13.25 h (0.552 d)
Sidereal rotation period
13.25 ± 0.2 h[5]
Geometric albedo
0.06–0.10[4]
Temperature~42 K
Absolute magnitude (H)
5.8,[4] 5.5[3]
Orbit and rotation
2001 YH140 is locked in 3:5 mean-motion resonance with Neptune. [4] When it makes three revolutions around the Sun, Neptune makes exactly five. The rotation period of (126154) 2001 YH140 is estimated to be 13.25 ± 0.2 hours. [5]
Physical characteristics
In 2010 thermal flux from (126154) 2001 YH140 in the far-infrared was measured by the Herschel Space Telescope. As a result, its size has been estimated to be 300–390 km (190–240 mi). [4]
References
1. "List Of Transneptunian Objects". IAU Minor Planet Center. Retrieved 2011-01-08.
2. "MPEC 2009-R09 :Distant Minor Planets (16 September 2009.0 TT)". IAU Minor Planet Center. 2009-09-04. Retrieved 2009-10-04.
3. "JPL Small-Body Database Browser: (126154) 2001 YH140" (last obs). 2009-02-02. Retrieved 11 April 2016.
4. Müller, T. G.; Lellouch, E.; Stansberry, J.; Kiss, C.; Santos-Sanz, P.; Vilenius, E.; Protopapa, S.; Moreno, R.; Mueller, M.; Delsanti, A.; Duffard, R.; Fornasier, S.; Groussin, O.; Harris, A. W.; Henry, F.; Horner, J.; Lacerda, P.; Lim, T.; Mommert, M.; Ortiz, J. L.; Rengel, M.; Thirouin, A.; Trilling, D.; Barucci, A.; Crovisier, J.; Doressoundiram, A.; Dotto, E.; Gutiérrez, P. J.; Hainaut, O. R.; Hartogh, P. (July–August 2010). ""TNOs are Cool": A survey of the trans-Neptunian region". Astronomy and Astrophysics. 518: L146. arXiv:1005.2923. Bibcode:2010A&A...518L.146M. doi:10.1051/0004-6361/201014683. S2CID 118635387.
5. Sheppard, Scott S. (August 2007). "Light Curves of Dwarf Plutonian Planets and other Large Kuiper Belt Objects: Their Rotations, Phase Functions, and Absolute Magnitudes". The Astronomical Journal. 134 (2): 787–798. arXiv:0704.1636. Bibcode:2007AJ....134..787S. doi:10.1086/519072. S2CID 56247384.
External links
• (126154) 2001 YH140 at the JPL Small-Body Database
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(126155) 2001 YJ140
(126155) 2001 YJ140 (provisional designation 2001 YJ140) is a resonant trans-Neptunian object from the outermost regions of the Solar System, approximately 154 kilometers in diameter. It discovered on 20 December 2001, by American astronomers Chad Trujillo, Glenn Smith and Michael E. Brown at the Palomar Observatory in California. [1]
(126154) 2001 YJ140
Discovery
Discovered byM. E. Brown
C. Trujillo
Glenn Smith
Discovery sitePalomar Obs.
Discovery date20 December 2001
Designations
MPC designation
(126155) 2001 YJ140
Alternative designations
none
Minor planet category
TNO · plutino
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc2455 days (6.72 yr)
Aphelion51.307 AU (7.6754 Tm)
Perihelion27.906 AU (4.1747 Tm)
Semi-major axis
39.606 AU (5.9250 Tm)
Eccentricity0.29542
Orbital period (sidereal)
249.26 yr (91043.2 d)
Mean anomaly
10.650°
Mean motion
0° 0m 14.235s / day
Inclination5.9691°
Longitude of ascending node
319.51°
Argument of perihelion
129.91°
Physical characteristics
Dimensions154 km (Johnston's Archive)
Absolute magnitude (H)
7.3
Orbit and rotation
2001 YJ140 is classified as a plutino, a large class of objects in a 2:3 orbital resonance with Neptune. Its orbit has a semi-major axis of 42.396 AU and an orbital period of about 249 years. Perihelion leads to 27.881 AU from the Sun and its aphelion in the distance of 51.348 AU. [2][3]
References
1. "JPL Small-Body Database Browser: 126155 (2001 YJ140)". NASA/Jet Propulsion Laboratory. Retrieved 7 April 2016.
2. MPEC 2009-R09 : DISTANT MINOR PLANETS (2009 SEPT. 16.0 TT)
3. List Of Transneptunian Objects
Sources
• NASA.gov
• IAU Minor Planet Center
External links
• (126155) 2001 YJ140 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (126155) 2001 YJ140 at the JPL Small-Body Database
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• (126154) 2001 YH140
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(131696) 2001 XT254
(131696) 2001 XT254, provisionally known as 2001 XT254, is a Kuiper belt object (KBO)[2] that has a 3:7 resonance with Neptune. [3]
(131696) 2001 XT254
Discovery[1]
Discovered bySheppard, S. S., Kleyna, J., Jewitt, D. C.
Discovery date9 December 2001
Designations
MPC designation
(131696) 2001 XT254
Minor planet category
SDO[2]
3:7 resonance[3][4]
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc4113 days (11.26 yr)
Aphelion70.889 AU (10.6048 Tm) (Q)
Perihelion35.892 AU (5.3694 Tm) (q)
Semi-major axis
53.391 AU (7.9872 Tm) (a)
Eccentricity0.32774 (e)
Orbital period (sidereal)
390.13 yr (142494 d)
Mean anomaly
359.98° (M)
Mean motion
0° 0m 9.095s / day (n)
Inclination0.51687° (i)
Longitude of ascending node
359.55° (Ω)
Argument of perihelion
133.36° (ω)
Earth MOID34.907 AU (5.2220 Tm)
Jupiter MOID30.5705 AU (4.57328 Tm)
Physical characteristics
Dimensions146 km (assumed)[5]
Geometric albedo
0.09 (assumed)
Absolute magnitude (H)
7.4[1]
It will come to perihelion in January 2016. [1]
Assuming a generic TNO albedo of 0.09, it is about 146 km in diameter. [5]
Resonance
Simulations by Emel’yanenko and Kiseleva in 2007 show that (131696) 2001 XT254 is librating in a 3:7 resonance with Neptune. [6] This libration can be stable for less than 100 million to billions of years. [6]
It has been observed 22 times over 4 oppositions. [1]
See also
(95625) 2002 GX32 has a similar resonant behavior.
References
1. "JPL Small-Body Database Browser: 131696 (2001 XT254)" (2006-01-29 last obs). Retrieved 7 April 2016.
2. "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2009-01-30.
3. Marc W. Buie. "Orbit Fit and Astrometric record for 131696" (2013-03-24 using 28 observations). SwRI (Space Science Department). Retrieved 2009-01-30.
4. "MPEC 2009-A63 :Distant Minor Planets (2009 JAN. 29.0 TT)". Minor Planet Center. 2009-01-13. Retrieved 2009-01-30.
5. Wm. Robert Johnston (22 August 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 13 February 2009. Retrieved 2009-01-30.
6. Emel’yanenko, V. V; Kiseleva, E. L. (2008). "Resonant motion of trans-Neptunian objects in high-eccentricity orbits". Astronomy Letters. 34 (4): 271–279. Bibcode:2008AstL...34..271E. doi:10.1134/S1063773708040075. S2CID 122634598.
External links
• (131696) 2001 XT254 at the JPL Small-Body Database
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• (131696) 2001 XT254
• (131697) 2001 XH255
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(131697) 2001 XH255
(131697) 2001 XH255, provisionally known as 2001 XH255, is a trans-Neptunian object (TNO) that has a 4:5 resonance with Neptune. [2]
(131697) 2001 XH255
Discovery[1]
Discovered by
• Kleyna, J.
• Sheppard, S. S.
• Jewitt, D. C.
Discovery date11 December 2001
Designations
MPC designation
(131697) 2001 XH255
Minor planet category
• TNO
• 4:5 resonance[2][3]
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc4110 days (11.25 yr)
Aphelion37.907 AU (5.6708 Tm) (Q)
Perihelion32.339 AU (4.8378 Tm) (q)
Semi-major axis
35.123 AU (5.2543 Tm) (a)
Eccentricity0.079253 (e)
Orbital period (sidereal)
208.16 yr (76030.5 d)
Mean anomaly
318.51° (M)
Mean motion
0° 0m 17.046s / day (n)
Inclination2.8512° (i)
Longitude of ascending node
323.17° (Ω)
Argument of perihelion
217.87° (ω)
Earth MOID31.3433 AU (4.68889 Tm)
Jupiter MOID26.8986 AU (4.02397 Tm)
Physical characteristics
Dimensions100 km (assumed)[4]
Geometric albedo
0.09 (assumed)
Apparent magnitude
23.6[5]
Absolute magnitude (H)
8.2[1]
It will come to perihelion in 2041. [1]
Assuming a generic TNO albedo of 0.09, it is about 100 km in diameter. [4]
Resonance
According to the Deep Ecliptic Survey and Minor Planet Center, (131697) 2001 XH255 has a 4:5 resonance with Neptune. [2][3] It comes as close as 32.2 AU from the Sun and has a fairly low orbital eccentricity of 0.07 with an inclination of only 2.86 degrees. [1]
The Neptune 4:5 resonance keeps it more than 7 AU from Neptune over a 14000-year period. [6]
It has been observed 21 times over 5 oppositions and has an orbit quality code of 3. [1]
Potential for Exploration
A NASA study in 2019 that confirmed the viability of using small radioisotope or nuclear fission power systems combined with xenon electric propulsion for deep space exploration, used 2001 XH255 as a representative Kuiper Belt Object as the mission's destination to orbit. [7]
References
1. "JPL Small-Body Database Browser: 131697 (2001 XH255)" (last observation: 2006-01-29). Retrieved 7 April 2016.
2. Marc W. Buie. "Orbit Fit and Astrometric record for 131697" (2006-01-29 using 19 observations). SwRI (Space Science Department). Retrieved 1 February 2009.
3. "MPEC 2009-A63 :Distant Minor Planets (2009 JAN. 29.0 TT)". Minor Planet Center. 13 January 2009. Retrieved 1 February 2009.
4. Wm. Robert Johnston (22 August 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 13 February 2009. Retrieved 1 February 2009.
5. "AstDys (131697) 2001XH255 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 26 May 2011. Retrieved 16 March 2009.
6. "MPEC 2006-H30 : 2001 XT254, 2001 XH255". Minor Planet Center. 22 April 2006. Retrieved 1 February 2009.
7. Oleson, S.; et al. (19 August 2019). "A Kuiper Belt Object Orbiter Enabled By 10 kW Kilopower Electric Propulsion" (PDF). NASA NTRS. Archived (PDF) from the original on 19 March 2020.
External links
• (131697) 2001 XH255 at the JPL Small-Body Database
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• (131697) 2001 XH255
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(13366) 1998 US24
(13366) 1998 US24 (provisional designation 1998 US24) is a Jupiter trojan from the Greek camp, approximately 33 kilometers (21 miles) in diameter. It was discovered on 18 October 1998, by astronomers with the Lowell Observatory Near-Earth-Object Search at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. [1] The dark Jovian asteroid is a slow rotator with a long rotation period of potentially 400 hours. [7] It has not been named since its numbering in January 2000. [8]
(13366) 1998 US24
Discovery[1]
Discovered byLONEOS
Discovery siteAnderson Mesa
Discovery date18 October 1998
Designations
MPC designation
(13366) 1998 US24
Alternative designations
1998 US24 · 1996 RX29
Minor planet category
Jupiter trojan[1][2]
Greek[3] · background[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc64.27 yr (23,476 d)
Aphelion5.7685 AU
Perihelion4.6895 AU
Semi-major axis
5.2290 AU
Eccentricity0.1032
Orbital period (sidereal)
11.96 yr (4,367 d)
Mean anomaly
193.23°
Mean motion
0° 4m 56.64s / day
Inclination6.6365°
Longitude of ascending node
96.296°
Argument of perihelion
355.47°
Jupiter MOID0.3771 AU
TJupiter2.9760
Physical characteristics
Mean diameter
33.30±2.87 km[5]
Synodic rotation period
400±105 h[6]
Geometric albedo
0.058±0.016[5]
Spectral type
C (assumed)[7]
Absolute magnitude (H)
11.10[5]
11.2[1][7]
11.3[2]
Orbit and classification
1998 US24 is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the leading Greek camp at the Gas Giant's L4 Lagrangian point, 60° ahead of its orbit (see Trojans in astronomy). [3] It is also a non-family asteroid in the Jovian background population. [4] It orbits the Sun at a distance of 4.7–5.8 AU once every 11 years and 12 months (4,367 days; semi-major axis of 5.23 AU). Its orbit has an eccentricity of 0.10 and an inclination of 7° with respect to the ecliptic. [2] The body's observation arc begins with a precovery taken at Palomar Observatory in February 1954, more than 44 years prior to its official discovery observation at Anderson Mesa. [1]
Numbering and naming
This minor planet was numbered by the MPC on 24 January 2000 (M.P.C. 37586). [8] As of 2018, it has not been named. [1]
Physical characteristics
1998 US24 is an assumed C-type asteroid, while most larger Jupiter trojans are D-types. [7]
Rotation period
In August 2015, a first rotational lightcurve of 1998 US24 was obtained from photometric observations by the Kepler space telescope during its K2 mission. Lightcurve analysis gave a rotation period of 400±105 hours with a brightness variation of 0.23 magnitude (U=2-). [6] One month later, a second, lower-rated lightcurve by Kepler determined an alternative period of 522±36 hours with an amplitude of 0.20 (U=1+). [9] As of 2018, no secure period of this slow rotator has yet been obtained. [7]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1998 US24 measures 33.30 kilometers in diameter and its surface has an albedo of 0.058,[5] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 32.03 kilometers based on an absolute magnitude of 11.2. [7]
100+ largest Jupiter trojans
Largest Jupiter Trojans by survey(A)
(mean-diameter in kilometers; YoD: Year of Discovery)
Designation H WISE IRAS Akari Ln RP V–I YoD Ref
624 Hektor7.2225233230.99L46.920.9301907list
617 Patroclus8.19140.362140.92140.85L5102.800.8301906list
911 Agamemnon7.89131.038166.66185.30L46.590.9801919list
588 Achilles8.67130.099135.47133.22L47.310.9401906list
3451 Mentor8.4126.288116.30117.91L57.700.7701984list
3317 Paris8.3118.790116.26120.45L57.090.9501984list
1867 Deiphobus8.3118.220122.67131.31L558.660.9301971list
1172 Äneas8.33118.020142.82148.66L58.710.9501930list
1437 Diomedes8.3117.786164.31172.60L424.490.8101937list
1143 Odysseus7.93114.624125.64130.81L410.110.8601930list
2241 Alcathous8.64113.682114.63118.87L57.690.9401979list
659 Nestor8.99112.320108.87107.06L415.980.7901908list
3793 Leonteus8.7112.04686.2687.58L45.620.7801985list
3063 Makhaon8.4111.655116.14114.34L48.640.8301983list
1583 Antilochus8.6108.842101.62111.69L431.540.9501950list
884 Priamus8.81101.09396.29119.99L56.860.9001917list
1208 Troilus8.99100.477103.34111.36L556.170.7401931list
1173 Anchises8.8999.549126.27120.49L511.600.7801930list
2207 Antenor8.8997.65885.1191.32L57.970.9501977list
2363 Cebriones9.1195.97681.8484.61L520.050.9101977list
4063 Euforbo8.795.619102.46106.38L48.850.9501989list
2357 Phereclos8.9494.62594.9098.45L514.390.9601981list
4709 Ennomos8.591.43380.8580.03L512.280.6901988list
2797 Teucer8.789.430111.14113.99L410.150.9201981list
2920 Automedon8.888.574111.01113.11L410.210.9501981list
15436 Dexius9.187.64685.7178.63L48.970.8701998list
3596 Meriones9.287.38075.0973.28L412.960.8301985list
2893 Peiroos9.2386.88487.4686.76L58.960.9501975list
4086 Podalirius9.185.49586.8985.98L410.430.8701985list
4060 Deipylos9.384.04379.2186.79L49.300.7601987list
1404 Ajax9.383.99081.6996.34L429.380.9601936list
4348 Poulydamas9.582.03270.0887.51L59.910.8401988list
5144 Achates9.080.95891.9189.85L55.960.9201991list
4833 Meges8.980.16587.3389.39L414.250.9401989list | 11 | 0 |
2223 Sarpedon9.4177.48094.63108.21L522.740.8801977list
4489 Dracius9.076.59592.9395.02L412.580.9501988list
2260 Neoptolemus9.3176.43571.6581.28L48.180.9501975list
5254 Ulysses9.276.14778.3480.00L428.720.9701986list
3708 Socus9.375.66179.5976.75L56.550.9801974list
2674 Pandarus9.174.26798.10101.72L58.481.0001982list
3564 Talthybius9.473.73068.9274.11L440.590.9001985list
4834 Thoas9.172.33186.8296.21L418.190.9501989list
7641 Cteatus9.471.83968.9775.28L427.770.9801986list
3540 Protesilaos9.370.22576.8487.66L48.950.9401973list
11395 Iphinous9.868.97764.7167.78L417.38–1998list
4035 Thestor9.668.73368.2366.99L413.470.9701986list
5264 Telephus9.468.47273.2681.38L49.530.9701991list
1868 Thersites9.568.16370.0878.89L410.480.9601960list
9799 Thronium9.668.03364.8772.42L421.520.9101996list
4068 Menestheus9.567.62562.3768.46L414.400.9501973list
23135 Pheidas9.966.23058.2968.50L48.690.8602000list
2456 Palamedes9.365.91691.6699.60L47.240.9201966list
3709 Polypoites9.165.29799.0985.23L410.041.0001985list
1749 Telamon9.564.89881.0669.14L416.980.9701949list
3548 Eurybates9.663.88572.1468.40L48.710.7301973list
4543 Phoinix9.763.83662.7969.54L438.871.2001989list
12444 Prothoon9.863.83564.3162.41L515.82–1996list
4836 Medon9.563.27767.7378.70L49.820.9201989list
16070 Charops9.763.19164.1368.98L520.240.9601999list
15440 Eioneus9.662.51966.4871.88L421.430.9701998list
4715 Medesicaste9.762.09763.9165.93L58.810.8501989list
34746 Thoon9.861.68460.5163.63L519.630.9502001list
38050 Bias9.861.60361.0450.44L418.850.9901998list
5130 Ilioneus9.760.71159.4052.49L514.770.9601989list
5027 Androgeos9.659.78657.86n.a.L411.380.9101988list
6090 Aulis9.459.56874.5381.92L418.480.9801989list
5648 Axius9.759.29563.91n.a.L537.560.9001990list
7119 Hiera9.759.15076.4077.29L44000.9501989list
4805 Asteropaios10.057.64753.1643.44L512.37–1990list
16974 Iphthime9.857.34155.4357.15L478.90.9601998list
4867 Polites9.857.25158.2964.29L511.241.0101989list
2895 Memnon10.056.70655.67n.a.L57.500.7101981list
4708 Polydoros9.954.96455.67n.a.L57.520.9601988list
(21601) 1998 XO8910.054.90955.6756.08L412.650.9701998list
12929 Periboea9.954.07761.0455.34L59.270.8801999list
17492 Hippasos10.053.97555.67n.a.L517.75–1991list
5652 Amphimachus10.153.92153.1652.48L48.371.0501992list
2759 Idomeneus9.953.67661.0152.55L432.380.9101980list
5258 Rhoeo10.253.27550.77n.a.L419.851.0101989list
(12126) 1999 RM1110.153.202n.a.n.a.L5n.a. ?1999list
(15502) 1999 NV2710.053.10055.6750.86L515.130.8751999list
4754 Panthoos10.053.02553.1556.96L527.68–1977list
4832 Palinurus10.052.05853.16n.a.L55.321.0001988list
5126 Achaemenides10.551.92244.2248.57L453.02–1989list
3240 Laocoon10.251.69550.77n.a.L511.310.8801978list
4902 Thessandrus9.851.26361.0471.79L47380.9601989list
11552 Boucolion10.151.13653.1653.91L532.44–1993list
(20729) 1999 XS14310.450.96146.30n.a.L45.721.0001999list
6545 Leitus10.150.95153.16n.a.L416.260.9101986list
4792 Lykaon10.150.87053.16n.a.L540.090.9601988list
21900 Orus10.050.81055.6753.87L413.450.9501999list
1873 Agenor10.150.79953.7654.38L520.60–1971list
5028 Halaesus10.250.77050.77n.a.L424.940.9001988list
2146 Stentor9.950.75558.29n.a.L416.40–1976list
4722 Agelaos10.050.37853.1659.47L518.440.9101977list
5284 Orsilocus10.150.15953.16n.a.L410.310.9701989list
11509 Thersilochos10.149.96053.1656.23L517.37–1990list
5285 Krethon10.149.60658.5352.61L412.041.0901989list
4791 Iphidamas10.149.52857.8559.96L59.701.0301988list
9023 Mnesthus10.149.15150.7760.80L530.66–1988list
5283 Pyrrhus9.748.35664.5869.93L47.320.9501989list
4946 Askalaphus10.248.20952.7166.10L422.730.9401988list
(22149) 2000 WD4910.248.19050.7750.37L47.841.0902000list
(32496) 2000 WX18210.248.01750.7751.63L523.340.9502000list
5120 Bitias10.247.98750.77n.a.L515.210.7801988list
12714 Alkimos10.147.81961.0454.62L428.48–1991list
7352 Hypsenor9.947.73155.67 47.07L56480.8501994list | 11 | 1 |
1870 Glaukos10.647.64942.23n.a.L55.99—1971list
4138 Kalchas10.146.46253.1661.04L429.20.8101973list
(23958) 1998 VD3010.246.00150.7747.91L45620.9901998list
4828 Misenus10.445.95446.30 43.22L512.870.9201988list
4057 Demophon10.145.68353.16n.a.L429.821.0601985list
4501 Eurypylos10.445.52446.30n.a.L46.05–1989list
4007 Euryalos10.345.51548.4853.89L46.39–1973list
5259 Epeigeus10.344.74142.5944.42L418.42–1989list
30705 Idaios10.444.54646.30n.a.L515.74–1977list
16560 Daitor10.743.86151.4243.38L5––1991list
(15977) 1998 MA1110.443.53046.3051.53L52500.9061998list
7543 Prylis10.642.89342.23n.a.L417.80–1973list
4827 Dares10.542.77044.22n.a.L519.00–1988list
1647 Menelaus10.542.71644.22n.a.L417.740.8661957list
(A) Used sources: WISE/NEOWISE catalog (NEOWISE_DIAM_V1 PDS, Grav, 2012); IRAS data (SIMPS v.6 catalog); and Akari catalog (Usui, 2011); RP: rotation period and V–I (color index) taken from the LCDB
Note: missing data was completed with figures from the JPL SBDB (query) and from the LCDB (query form) for the WISE/NEOWISE and SIMPS catalogs, respectively. These figures are given in italics. Also, listing is incomplete above #100.
References
1. "13366 (1998 US24)". Minor Planet Center. Retrieved 4 July 2018.
2. "JPL Small-Body Database Browser: 13366 (1998 US24)" (2018-05-21 last obs.). Jet Propulsion Laboratory. Retrieved 4 July 2018.
3. "List of Jupiter Trojans". Minor Planet Center. 1 July 2018. Retrieved 4 July 2018.
4. "Asteroid (13366) 1998 US24 – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 4 July 2018.
5. Grav, T.; Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.; Nugent, C. R. (November 2012). "WISE/NEOWISE Observations of the Jovian Trojan Population: Taxonomy". The Astrophysical Journal. 759 (1): 10. arXiv:1209.1549. Bibcode:2012ApJ...759...49G. doi:10.1088/0004-637X/759/1/49. S2CID 119101711. (online catalog)
6. Szabó, Gy. M.; Pál, A.; Kiss, Cs. ; Kiss, L. L.; Molnár, L.; Hanyecz, O.; et al. (March 2017). "The heart of the swarm: K2 photometry and rotational characteristics of 56 Jovian Trojan asteroids". Astronomy and Astrophysics. 599: 13. arXiv:1609.02760. Bibcode:2017A&A...599A..44S. doi:10.1051/0004-6361/201629401. S2CID 119275951.
7. "LCDB Data for (13366)". Asteroid Lightcurve Database (LCDB). Retrieved 4 July 2018.
8. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 July 2018.
9. Ryan, Erin Lee; Sharkey, Benjamin N. L.; Woodward, Charles E. (March 2017). "Trojan Asteroids in the Kepler Campaign 6 Field". The Astronomical Journal. 153 (3): 12. Bibcode:2017AJ....153..116R. doi:10.3847/1538-3881/153/3/116. S2CID 125570438.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (10001)-(15000) – Minor Planet Center
• Asteroid (13366) 1998 US24 at the Small Bodies Data Ferret
• (13366) 1998 US24 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (13366) 1998 US24 at the JPL Small-Body Database
Minor planets navigator
• 13365 Tenzinyama
• (13366) 1998 US24
• 13367 Jiří
Small Solar System bodies
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• Designation
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• MPC | 11 | 2 |
Pluto
Pluto (minor-planet designation: 134340 Pluto) is a dwarf planet in the Kuiper belt, a ring of bodies beyond the orbit of Neptune. It is the ninth-largest and tenth-most-massive known object to directly orbit the Sun. It is the largest known trans-Neptunian object by volume, by a small margin, but is less massive than Eris. Like other Kuiper belt objects, Pluto is made primarily of ice and rock and is much smaller than the inner planets. Pluto has roughly one-sixth the mass of Earth's moon, and one-third its volume.
134340 Pluto
Pluto, imaged by the New Horizons spacecraft, July 2015. [lower-alpha 1] The most prominent feature in the image, the bright, youthful plains of Tombaugh Regio and Sputnik Planitia, can be seen at right. It contrasts the darker, cratered terrain of Belton Regio at lower left
Discovery
Discovered byClyde W. Tombaugh
Discovery siteLowell Observatory
Discovery dateFebruary 18, 1930
Designations
Designation
(134340) Pluto
Pronunciation/ˈpluːtoʊ/
Named after
Pluto
Minor planet category
• Dwarf planet
• Trans-Neptunian object
• Kuiper belt object
• Plutino
AdjectivesPlutonian /pluːˈtoʊniən/[1]
Symbol (historically astronomical, now mostly astrological) or (mostly astrological)
Orbital characteristics[2][lower-alpha 2]
Epoch J2000
Earliest precovery dateAugust 20, 1909
Aphelion
• 49.305 AU
• (7.37593 billion km)
• February 2114
Perihelion
• 29.658 AU
• (4.43682 billion km)[3]
• (September 5, 1989)[4]
Semi-major axis
• 39.482 AU
• (5.90638 billion km)
Eccentricity0.2488
Orbital period (sidereal)
• 247.94 years[3]
• 90,560 d[3]
Orbital period (synodic)
366.73 days[3]
Average orbital speed
4.743 km/s[3]
Mean anomaly
14.53 deg
Inclination
• 17.16°
• (11.88° to Sun's equator)
Longitude of ascending node
110.299°
Argument of perihelion
113.834°
Known satellites5
Physical characteristics
Dimensions2,376.6±1.6 km (observations consistent with a sphere, predicted deviations too small to be observed)[5]
Mean radius
• 1,188.3±0.8 km[6][5]
• 0.1868 Earths
Flattening<1%[7]
Surface area
• 1.774443×107 km2[lower-alpha 3]
• 0.035 Earths
Volume
• (7.057±0.004)×109 km3[lower-alpha 4]
• 0.00651 Earths
Mass
• (1.3025±0.0006)×1022 kg[8]
• 0.00218 Earths
• 0.177 Moons
Mean density
1.853±0.004 g/cm3[8]
Surface gravity
0.620 m/s2 (0.0632 g0)[lower-alpha 5]
Escape velocity
1.212 km/s[lower-alpha 6]
Synodic rotation period
• −6.38680 d
• −6 d, 9 h, 17 m, 00 s
[9]
Sidereal rotation period
• −6.387230 d
• −6 d, 9 h, 17 m, 36 s
Equatorial rotation velocity
47.18 km/h
Axial tilt
122.53° (to orbit)[3]
North pole right ascension
132.993°[10]
North pole declination
−6.163°[10]
Albedo0.52 geometric[3]
0.72 Bond[3]
Surface temp. min mean max
Kelvin 33 K 44 K (−229 °C) 55 K
Apparent magnitude
13.65[3] to 16.3[11]
(mean is 15.1)[3]
Absolute magnitude (H)
−0.44[12]
Angular diameter
0.06″ to 0.11″[3][lower-alpha 7]
Atmosphere
Surface pressure
1.0 Pa (2015)[7][13]
Composition by volumeNitrogen, methane, carbon monoxide[14]
Pluto has a moderately eccentric and inclined orbit, ranging from 30 to 49 astronomical units (4.5 to 7.3 billion kilometers; 2.8 to 4.6 billion miles) from the Sun. Light from the Sun takes 5.5 hours to reach Pluto at its orbital distance of 39.5 AU (5.91 billion km; 3.67 billion mi). Pluto's eccentric orbit periodically brings it closer to the Sun than Neptune, but a stable orbital resonance prevents them from colliding.
Pluto has five known moons: Charon, the largest, whose diameter is just over half that of Pluto; Styx; Nix; Kerberos; and Hydra. Pluto and Charon are sometimes considered a binary system because the barycenter of their orbits does not lie within either body, and they are tidally locked. The New Horizons mission was the first spacecraft to visit Pluto and its moons, making a flyby on July 14, 2015, and taking detailed measurements and observations.
Pluto was discovered in 1930 by Clyde W. Tombaugh, making it by far the first known object in the Kuiper belt. It was immediately hailed as the ninth planet, but it was always the odd object out,[15]: 27 and its planetary status was questioned when it was found to be much smaller than expected. These doubts increased following the discovery of additional objects in the Kuiper belt starting in the 1990s, and particularly the more massive scattered disk object Eris in 2005. In 2006, the International Astronomical Union (IAU) formally redefined the term planet to exclude dwarf planets such as Pluto. Many planetary astronomers, however, continue to consider Pluto and other dwarf planets to be planets.
History
Discovery
Further information: Planets beyond Neptune
In the 1840s, Urbain Le Verrier used Newtonian mechanics to predict the position of the then-undiscovered planet Neptune after analyzing perturbations in the orbit of Uranus. Subsequent observations of Neptune in the late 19th century led astronomers to speculate that Uranus's orbit was being disturbed by another planet besides Neptune. [16]
In 1906, Percival Lowell—a wealthy Bostonian who had founded Lowell Observatory in Flagstaff, Arizona, in 1894—started an extensive project in search of a possible ninth planet, which he termed "Planet X". [17] By 1909, Lowell and William H. Pickering had suggested several possible celestial coordinates for such a planet. [18] Lowell and his observatory conducted his search, using mathematical calculations made by Elizabeth Williams, until his death in 1916, but to no avail. Unknown to Lowell, his surveys had captured two faint images of Pluto on March 19 and April 7, 1915, but they were not recognized for what they were. [18][19] There are fourteen other known precovery observations, with the earliest made by the Yerkes Observatory on August 20, 1909. [20]
Percival's widow, Constance Lowell, entered into a ten-year legal battle with the Lowell Observatory over her husband's legacy, and the search for Planet X did not resume until 1929. [21] Vesto Melvin Slipher, the observatory director, gave the job of locating Planet X to 23-year-old Clyde Tombaugh, who had just arrived at the observatory after Slipher had been impressed by a sample of his astronomical drawings. [21]
Tombaugh's task was to systematically image the night sky in pairs of photographs, then examine each pair and determine whether any objects had shifted position. Using a blink comparator, he rapidly shifted back and forth between views of each of the plates to create the illusion of movement of any objects that had changed position or appearance between photographs. On February 18, 1930, after nearly a year of searching, Tombaugh discovered a possible moving object on photographic plates taken on January 23 and 29. A lesser-quality photograph taken on January 21 helped confirm the movement. [22] After the observatory obtained further confirmatory photographs, news of the discovery was telegraphed to the Harvard College Observatory on March 13, 1930. [18] | 12 | 0 |
One Plutonian year corresponds to 247.94 Earth years;[3] thus, in 2178, Pluto will complete its first orbit since its discovery.
Name and symbol
The name Pluto came from the Roman god of the underworld; and it is also an epithet for Hades (the Greek equivalent of Pluto).
Upon the announcement of the discovery, Lowell Observatory received over a thousand suggestions for names. [23] Three names topped the list: Minerva, Pluto and Cronus. 'Minerva' was the Lowell staff's first choice[24] but was rejected because it had already been used for an asteroid; Cronus was disfavored because it was promoted by an unpopular and egocentric astronomer, Thomas Jefferson Jackson See. A vote was then taken and 'Pluto' was the unanimous choice. To make sure the name stuck, and that the planet would not suffer changes in its name as Uranus had, Lowell Observatory proposed the name to the American Astronomical Society and the Royal Astronomical Society; both approved it unanimously. [15]: 136 [25] The name was published on May 1, 1930. [26][27]
The name Pluto had received some 150 nominations among the letters and telegrams sent to Lowell. The first[lower-alpha 8] had been from Venetia Burney (1918–2009), an eleven-year-old schoolgirl in Oxford, England, who was interested in classical mythology. [15][26] She had suggested it to her grandfather Falconer Madan when he read the news of Pluto's discovery to his family over breakfast; Madan passed the suggestion to astronomy professor Herbert Hall Turner, who cabled it to colleagues at Lowell on March 16, three days after the announcement. [24][26]
The name 'Pluto' was mythologically appropriate: the god Pluto was one of six surviving children of Saturn, and the others had already all been chosen as names of major or minor planets (his brothers Jupiter and Neptune, and his sisters Ceres, Juno and Vesta). Both the god and the planet inhabited "gloomy" regions, and the god was able to make himself invisible, as the planet had been for so long. [29] The choice was further helped by the fact that the first two letters of Pluto were the initials of Percival Lowell; indeed, 'Percival' had been one of the more popular suggestions for a name for the new planet. [24][30] Pluto's planetary symbol ⟨⟩ was then created as a monogram of the letters "PL". [31] This symbol is rarely used in astronomy anymore,[lower-alpha 9] though it is still common in astrology. However, the most common astrological symbol for Pluto, occasionally used in astronomy as well, is an orb (possibly representing Pluto's invisibility cap) over Pluto's bident ⟨⟩, which dates to the early 1930s. [35][lower-alpha 10]
The name 'Pluto' was soon embraced by wider culture. In 1930, Walt Disney was apparently inspired by it when he introduced for Mickey Mouse a canine companion named Pluto, although Disney animator Ben Sharpsteen could not confirm why the name was given. [39] In 1941, Glenn T. Seaborg named the newly created element plutonium after Pluto, in keeping with the tradition of naming elements after newly discovered planets, following uranium, which was named after Uranus, and neptunium, which was named after Neptune. [40]
Most languages use the name "Pluto" in various transliterations. [lower-alpha 11] In Japanese, Houei Nojiri suggested the calque Meiōsei (冥王星, "Star of the King (God) of the Underworld"), and this was borrowed into Chinese and Korean. Some languages of India use the name Pluto, but others, such as Hindi, use the name of Yama, the God of Death in Hinduism. [41] Polynesian languages also tend to use the indigenous god of the underworld, as in Māori Whiro. [41] Vietnamese might be expected to follow Chinese, but does not because the Sino-Vietnamese word 冥 minh "dark" is homophonous with 明 minh "bright". Vietnamese instead uses Yama, which is also a Buddhist deity, in the form of Sao Diêm Vương 星閻王 "Yama's Star", derived from Chinese 閻王 Yán Wáng / Yìhm Wòhng "King Yama". [41][42][43]
Planet X disproved
Once Pluto was found, its faintness and lack of a viewable disc cast doubt on the idea that it was Lowell's Planet X. [17] Estimates of Pluto's mass were revised downward throughout the 20th century. [44]
Mass estimates for Pluto
Year Mass Estimate by
1915
7 Earths
Lowell (prediction for Planet X)[17]
1931
1 Earth
Nicholson & Mayall[45][46][47]
1948
0.1 (1/10) Earth
Kuiper[48]
1976
0.01 (1/100) Earth
Cruikshank, Pilcher, & Morrison[49]
1978
0.0015 (1/650) Earth
Christy & Harrington[50]
2006
0.00218 (1/459) Earth
Buie et al. [51]
Astronomers initially calculated its mass based on its presumed effect on Neptune and Uranus. In 1931, Pluto was calculated to be roughly the mass of Earth, with further calculations in 1948 bringing the mass down to roughly that of Mars. [46][48] In 1976, Dale Cruikshank, Carl Pilcher and David Morrison of the University of Hawaiʻi calculated Pluto's albedo for the first time, finding that it matched that for methane ice; this meant Pluto had to be exceptionally luminous for its size and therefore could not be more than 1 percent the mass of Earth. [49] (Pluto's albedo is 1.4–1.9 times that of Earth. [3])
In 1978, the discovery of Pluto's moon Charon allowed the measurement of Pluto's mass for the first time: roughly 0.2% that of Earth, and far too small to account for the discrepancies in the orbit of Uranus. Subsequent searches for an alternative Planet X, notably by Robert Sutton Harrington,[52] failed. In 1992, Myles Standish used data from Voyager 2's flyby of Neptune in 1989, which had revised the estimates of Neptune's mass downward by 0.5%—an amount comparable to the mass of Mars—to recalculate its gravitational effect on Uranus. With the new figures added in, the discrepancies, and with them the need for a Planet X, vanished. [53] As of 2000 the majority of scientists agree that Planet X, as Lowell defined it, does not exist. [54] Lowell had made a prediction of Planet X's orbit and position in 1915 that was fairly close to Pluto's actual orbit and its position at that time; Ernest W. Brown concluded soon after Pluto's discovery that this was a coincidence. [55]
Classification
Further information: Definition of planet
From 1992 onward, many bodies were discovered orbiting in the same volume as Pluto, showing that Pluto is part of a population of objects called the Kuiper belt. This made its official status as a planet controversial, with many questioning whether Pluto should be considered together with or separately from its surrounding population. Museum and planetarium directors occasionally created controversy by omitting Pluto from planetary models of the Solar System. In February 2000 the Hayden Planetarium in New York City displayed a Solar System model of only eight planets, which made headlines almost a year later. [56]
Ceres, Pallas, Juno and Vesta lost their planet status among most astronomers after the discovery of many other asteroids. On the other hand, planetary geologists often regarded Ceres, and less often Pallas and Vesta, as being different from smaller asteroids because they were large enough to have undergone geological evolution. [57] Although the first Kuiper belt objects discovered were quite small, objects increasingly closer in size to Pluto were soon discovered, some large enough (like Pluto itself) to satisfy geological but not dynamical ideas of planethood. [58] On July 29, 2005, the debate became unavoidable, astronomers at Caltech announced the discovery of a new trans-Neptunian object, Eris, which was substantially more massive than Pluto and the most massive object discovered in the Solar System since Triton in 1846. Its discoverers and the press initially called it the tenth planet, although there was no official consensus at the time on whether to call it a planet. [59] Others in the astronomical community considered the discovery the strongest argument for reclassifying Pluto as a minor planet. [60]
IAU classification
Main article: IAU definition of planet
The debate came to a head in August 2006, with an IAU resolution that created an official definition for the term "planet". According to this resolution, there are three conditions for an object in the Solar System to be considered a planet:
• The object must be in orbit around the Sun.
• The object must be massive enough to be rounded by its own gravity. More specifically, its own gravity should pull it into a shape defined by hydrostatic equilibrium.
• It must have cleared the neighborhood around its orbit. [61][62] | 12 | 1 |
Pluto fails to meet the third condition. [63] Its mass is substantially less than the combined mass of the other objects in its orbit: 0.07 times, in contrast to Earth, which is 1.7 million times the remaining mass in its orbit (excluding the moon). [64][62] The IAU further decided that bodies that, like Pluto, meet criteria 1 and 2, but do not meet criterion 3 would be called dwarf planets. In September 2006, the IAU included Pluto, and Eris and its moon Dysnomia, in their Minor Planet Catalogue, giving them the official minor-planet designations "(134340) Pluto", "(136199) Eris", and "(136199) Eris I Dysnomia". [65] Had Pluto been included upon its discovery in 1930, it would have likely been designated 1164, following 1163 Saga, which was discovered a month earlier. [66]
There has been some resistance within the astronomical community toward the reclassification, and in particular planetary scientists often continue to reject it, considering Pluto, Charon, and Eris to be planets for the same reason they do so for Ceres. In effect, this amounts to accepting only the second clause of the IAU definition. [67][68][69] Alan Stern, principal investigator with NASA's New Horizons mission to Pluto, derided the IAU resolution. [70][71] He also stated that because less than five percent of astronomers voted for it, the decision was not representative of the entire astronomical community. [71] Marc W. Buie, then at the Lowell Observatory, petitioned against the definition. [72] Others have supported the IAU, for example Mike Brown, the astronomer who discovered Eris. [73]
Public reception to the IAU decision was mixed. A resolution introduced in the California State Assembly facetiously called the IAU decision a "scientific heresy". [74] The New Mexico House of Representatives passed a resolution in honor of Clyde Tombaugh, the discoverer of Pluto and a longtime resident of that state, that declared that Pluto will always be considered a planet while in New Mexican skies and that March 13, 2007 was Pluto Planet Day. [75][76] The Illinois Senate passed a similar resolution in 2009 on the basis that Tombaugh was born in Illinois. The resolution asserted that Pluto was "unfairly downgraded to a 'dwarf' planet" by the IAU. "[77] Some members of the public have also rejected the change, citing the disagreement within the scientific community on the issue, or for sentimental reasons, maintaining that they have always known Pluto as a planet and will continue to do so regardless of the IAU decision. [78] In 2006, in its 17th annual words-of-the-year vote, the American Dialect Society voted plutoed as the word of the year. To "pluto" is to "demote or devalue someone or something". [79]
Researchers on both sides of the debate gathered in August 2008, at the Johns Hopkins University Applied Physics Laboratory for a conference that included back-to-back talks on the IAU definition of a planet. [80] Entitled "The Great Planet Debate",[81] the conference published a post-conference press release indicating that scientists could not come to a consensus about the definition of planet. [82] In June 2008, the IAU had announced in a press release that the term "plutoid" would henceforth be used to refer to Pluto and other planetary-mass objects that have an orbital semi-major axis greater than that of Neptune, though the term has not seen significant use. [83][84][85]
In April 2024, Arizona (where Pluto was first discovered in 1930) passed a law naming Pluto as the official state planet. [86]
Orbit
Pluto's orbital period is about 248 years. Its orbital characteristics are substantially different from those of the planets, which follow nearly circular orbits around the Sun close to a flat reference plane called the ecliptic. In contrast, Pluto's orbit is moderately inclined relative to the ecliptic (over 17°) and moderately eccentric (elliptical). This eccentricity means a small region of Pluto's orbit lies closer to the Sun than Neptune's. The Pluto–Charon barycenter came to perihelion on September 5, 1989,[4][lower-alpha 12] and was last closer to the Sun than Neptune between February 7, 1979, and February 11, 1999. [87]
Although the 3:2 resonance with Neptune (see below) is maintained, Pluto's inclination and eccentricity behave in a chaotic manner. Computer simulations can be used to predict its position for several million years (both forward and backward in time), but after intervals much longer than the Lyapunov time of 10–20 million years, calculations become unreliable: Pluto is sensitive to immeasurably small details of the Solar System, hard-to-predict factors that will gradually change Pluto's position in its orbit. [88][89]
The semi-major axis of Pluto's orbit varies between about 39.3 and 39.6 AU with a period of about 19,951 years, corresponding to an orbital period varying between 246 and 249 years. The semi-major axis and period are presently getting longer. [90]
Relationship with Neptune
Despite Pluto's orbit appearing to cross that of Neptune when viewed from north or south of the Solar System, the two objects' orbits do not intersect. When Pluto is closest to the Sun, and close to Neptune's orbit as viewed from such a position, it is also the farthest north of Neptune's path. Pluto's orbit passes about 8 AU north of that of Neptune, preventing a collision. [91][92][93][lower-alpha 13]
This alone is not enough to protect Pluto; perturbations from the planets (especially Neptune) could alter Pluto's orbit (such as its orbital precession) over millions of years so that a collision could happen. However, Pluto is also protected by its 2:3 orbital resonance with Neptune: for every two orbits that Pluto makes around the Sun, Neptune makes three, in a frame of reference that rotates at the rate that Pluto's perihelion precesses (about 0.97×10−4 degrees per year[90]). Each cycle lasts about 495 years. (There are many other objects in this same resonance, called plutinos.) At present, in each 495-year cycle, the first time Pluto is at perihelion (such as in 1989), Neptune is 57° ahead of Pluto. By Pluto's second passage through perihelion, Neptune will have completed a further one and a half of its own orbits, and will be 123° behind Pluto. [95] Pluto and Neptune's minimum separation is over 17 AU, which is greater than Pluto's minimum separation from Uranus (11 AU). [93] The minimum separation between Pluto and Neptune actually occurs near the time of Pluto's aphelion. [90]
The 2:3 resonance between the two bodies is highly stable and has been preserved over millions of years. [96] This prevents their orbits from changing relative to one another, so the two bodies can never pass near each other. Even if Pluto's orbit were not inclined, the two bodies could never collide. [93] When Pluto's period is slightly different from 3/2 of Neptune's, the pattern of its distance from Neptune will drift. Near perihelion Pluto moves interior to Neptune's orbit and is therefore moving faster, so during the first of two orbits in the 495-year cycle, it is approaching Neptune from behind. At present it remains between 50° and 65° behind Neptune for 100 years (e.g. 1937–2036). [95] The gravitational pull between the two causes angular momentum to be transferred to Pluto. This situation moves Pluto into a slightly larger orbit, where it has a slightly longer period, according to Kepler's third law. After several such repetitions, Pluto is sufficiently delayed that at the second perihelion of each cycle it will not be far ahead of Neptune coming behind it, and Neptune will start to decrease Pluto's period again. The whole cycle takes about 20,000 years to complete. [93][96][97]
Other factors
Numerical studies have shown that over millions of years, the general nature of the alignment between the orbits of Pluto and Neptune does not change. [91][90] There are several other resonances and interactions that enhance Pluto's stability. These arise principally from two additional mechanisms (besides the 2:3 mean-motion resonance).
First, Pluto's argument of perihelion, the angle between the point where it crosses the ecliptic (or the invariant plane) and the point where it is closest to the Sun, librates around 90°. [90] This means that when Pluto is closest to the Sun, it is at its farthest north of the plane of the Solar System, preventing encounters with Neptune. This is a consequence of the Kozai mechanism,[91] which relates the eccentricity of an orbit to its inclination to a larger perturbing body—in this case, Neptune. Relative to Neptune, the amplitude of libration is 38°, and so the angular separation of Pluto's perihelion to the orbit of Neptune is always greater than 52° (90°–38°). The closest such angular separation occurs every 10,000 years. [96] | 12 | 2 |
Second, the longitudes of ascending nodes of the two bodies—the points where they cross the invariant plane—are in near-resonance with the above libration. When the two longitudes are the same—that is, when one could draw a straight line through both nodes and the Sun—Pluto's perihelion lies exactly at 90°, and hence it comes closest to the Sun when it is furthest north of Neptune's orbit. This is known as the 1:1 superresonance. All the Jovian planets (Jupiter, Saturn, Uranus, and Neptune) play a role in the creation of the superresonance. [91]
Orcus
The 2nd-largest known plutino, Orcus, has a diameter around 900 km and is in a very similar orbit to that of Pluto. However, the orbits of Pluto and Orcus are out of phase, so that the two never approach each other. It has been termed the "anti-Pluto", and is named for the Etruscan counterpart to the god Pluto.
Rotation
Pluto's rotation period, its day, is equal to 6.387 Earth days. [3][98] Like Uranus and 2 Pallas, Pluto rotates on its "side" in its orbital plane, with an axial tilt of 120°, and so its seasonal variation is extreme; at its solstices, one-fourth of its surface is in continuous daylight, whereas another fourth is in continuous darkness. [99] The reason for this unusual orientation has been debated. Research from the University of Arizona has suggested that it may be due to the way that a body's spin will always adjust to minimise energy. This could mean a body reorienting itself to put extraneous mass near the equator and regions lacking mass tend towards the poles. This is called polar wander. [100] According to a paper released from the University of Arizona, this could be caused by masses of frozen nitrogen building up in shadowed areas of the dwarf planet. These masses would cause the body to reorient itself, leading to its unusual axial tilt of 120°. The buildup of nitrogen is due to Pluto's vast distance from the Sun. At the equator, temperatures can drop to −240 °C (−400.0 °F; 33.1 K), causing nitrogen to freeze as water would freeze on Earth. The same polar wandering effect seen on Pluto would be observed on Earth were the Antarctic ice sheet several times larger. [101]
Geology
Main articles: Geology of Pluto and Geography of Pluto
Surface
The plains on Pluto's surface are composed of more than 98 percent nitrogen ice, with traces of methane and carbon monoxide. [102] Nitrogen and carbon monoxide are most abundant on the anti-Charon face of Pluto (around 180° longitude, where Tombaugh Regio's western lobe, Sputnik Planitia, is located), whereas methane is most abundant near 300° east. [103] The mountains are made of water ice. [104] Pluto's surface is quite varied, with large differences in both brightness and color. [105] Pluto is one of the most contrastive bodies in the Solar System, with as much contrast as Saturn's moon Iapetus. [106] The color varies from charcoal black, to dark orange and white. [107] Pluto's color is more similar to that of Io with slightly more orange and significantly less red than Mars. [108] Notable geographical features include Tombaugh Regio, or the "Heart" (a large bright area on the side opposite Charon), Belton Regio,[6] or the "Whale" (a large dark area on the trailing hemisphere), and the "Brass Knuckles" (a series of equatorial dark areas on the leading hemisphere).
Sputnik Planitia, the western lobe of the "Heart", is a 1,000 km-wide basin of frozen nitrogen and carbon monoxide ices, divided into polygonal cells, which are interpreted as convection cells that carry floating blocks of water ice crust and sublimation pits towards their margins;[109][110][111] there are obvious signs of glacial flows both into and out of the basin. [112][113] It has no craters that were visible to New Horizons, indicating that its surface is less than 10 million years old. [114] Latest studies have shown that the surface has an age of 180000+90000
−40000 years. [115] The New Horizons science team summarized initial findings as "Pluto displays a surprisingly wide variety of geological landforms, including those resulting from glaciological and surface–atmosphere interactions as well as impact, tectonic, possible cryovolcanic, and mass-wasting processes. "[7]
In Western parts of Sputnik Planitia there are fields of transverse dunes formed by the winds blowing from the center of Sputnik Planitia in the direction of surrounding mountains. The dune wavelengths are in the range of 0.4–1 km and likely consist of methane particles 200–300 μm in size. [116]
• Multispectral Visual Imaging Camera image of Pluto in enhanced color to bring out differences in surface composition.
• Distribution of numerous impact craters and basins on both Pluto and Charon. The variation in density (with none found in Sputnik Planitia) indicates a long history of varying geological activity. Precisely for this reason, the confidence of numerous craters on Pluto remain uncertain. [117] The lack of craters on the left and right of each map is due to low-resolution coverage of those anti-encounter regions.
• Geologic map of Sputnik Planitia and surroundings (context), with convection cell margins outlined in black
• Regions where water ice has been detected (blue regions)
Internal structure
"Life on Pluto" redirects here. For fiction about aliens from Pluto, see Life on Pluto in fiction.
Pluto's density is 1.853±0.004 g/cm3. [8] Because the decay of radioactive elements would eventually heat the ices enough for the rock to separate from them, scientists expect that Pluto's internal structure is differentiated, with the rocky material having settled into a dense core surrounded by a mantle of water ice. The pre–New Horizons estimate for the diameter of the core is 1700 km, 70% of Pluto's diameter. [118] It is possible that such heating continues, creating a subsurface ocean of liquid water 100 to 180 km thick at the core–mantle boundary. [118][119][120] In September 2016, scientists at Brown University simulated the impact thought to have formed Sputnik Planitia, and showed that it might have been the result of liquid water upwelling from below after the collision, implying the existence of a subsurface ocean at least 100 km deep. [121] In June 2020, astronomers reported evidence that Pluto may have had a subsurface ocean, and consequently may have been habitable, when it was first formed. [122][123] In March 2022, a team of researchers proposed that the mountains Wright Mons and Piccard Mons are actually a merger of many smaller cryovolcanic domes, suggesting a source of heat on the body at levels previously thought not possible. [124]
Mass and size
Pluto's diameter is 2376.6±3.2 km[5] and its mass is (1.303±0.003)×1022 kg, 17.7% that of the Moon (0.22% that of Earth). [125] Its surface area is 1.774443×107 km2, or just slightly bigger than Russia or Antarctica (particularly including the Antarctic sea ice during winter). Its surface gravity is 0.063 g (compared to 1 g for Earth and 0.17 g for the Moon). [3] This gives Pluto an escape velocity of 4,363.2 km per hour / 2,711.167 miles per hour (as compared to Earth's 40,270 km per hour / 25,020 miles per hour). Pluto is more than twice the diameter and a dozen times the mass of Ceres, the largest object in the asteroid belt. It is less massive than the dwarf planet Eris, a trans-Neptunian object discovered in 2005, though Pluto has a larger diameter of 2,376.6 km[5] compared to Eris's approximate diameter of 2,326 km. [126]
With less than 0.2 lunar masses, Pluto is much less massive than the terrestrial planets, and also less massive than seven moons: Ganymede, Titan, Callisto, Io, the Moon, Europa, and Triton. The mass is much less than thought before Charon was discovered. [127]
The discovery of Pluto's satellite Charon in 1978 enabled a determination of the mass of the Pluto–Charon system by application of Newton's formulation of Kepler's third law. Observations of Pluto in occultation with Charon allowed scientists to establish Pluto's diameter more accurately, whereas the invention of adaptive optics allowed them to determine its shape more accurately. [128]
Determinations of Pluto's size have been complicated by its atmosphere[129] and hydrocarbon haze. [130] In March 2014, Lellouch, de Bergh et al. | 12 | 3 |
published findings regarding methane mixing ratios in Pluto's atmosphere consistent with a Plutonian diameter greater than 2,360 km, with a "best guess" of 2,368 km. [131] On July 13, 2015, images from NASA's New Horizons mission Long Range Reconnaissance Imager (LORRI), along with data from the other instruments, determined Pluto's diameter to be 2,370 km (1,473 mi),[126][132] which was later revised to be 2,372 km (1,474 mi) on July 24,[133] and later to 2374±8 km. [7] Using radio occultation data from the New Horizons Radio Science Experiment (REX), the diameter was found to be 2376.6±3.2 km. [5]
The masses of Pluto and Charon compared to other dwarf planets (Eris, Haumea, Makemake, Gonggong, Quaoar, Orcus, Ceres) and to the icy moons Triton (Neptune I), Titania (Uranus III), Oberon (Uranus IV), Rhea (Saturn V) and Iapetus (Saturn VIII). The unit of mass is ×1021 kg.
Atmosphere
Main article: Atmosphere of Pluto
Pluto has a tenuous atmosphere consisting of nitrogen (N2), methane (CH4), and carbon monoxide (CO), which are in equilibrium with their ices on Pluto's surface. [134][135] According to the measurements by New Horizons, the surface pressure is about 1 Pa (10 μbar),[7] roughly one million to 100,000 times less than Earth's atmospheric pressure. It was initially thought that, as Pluto moves away from the Sun, its atmosphere should gradually freeze onto the surface; studies of New Horizons data and ground-based occultations show that Pluto's atmospheric density increases, and that it likely remains gaseous throughout Pluto's orbit. [136][137] New Horizons observations showed that atmospheric escape of nitrogen to be 10,000 times less than expected. [137] Alan Stern has contended that even a small increase in Pluto's surface temperature can lead to exponential increases in Pluto's atmospheric density; from 18 hPa to as much as 280 hPa (three times that of Mars to a quarter that of the Earth). At such densities, nitrogen could flow across the surface as liquid. [137] Just like sweat cools the body as it evaporates from the skin, the sublimation of Pluto's atmosphere cools its surface. [138] Pluto has no or almost no troposphere; observations by New Horizons suggest only a thin tropospheric boundary layer. Its thickness in the place of measurement was 4 km, and the temperature was 37±3 K. The layer is not continuous. [139]
In July 2019, an occultation by Pluto showed that its atmospheric pressure, against expectations, had fallen by 20% since 2016. [140] In 2021, astronomers at the Southwest Research Institute confirmed the result using data from an occultation in 2018, which showed that light was appearing less gradually from behind Pluto's disc, indicating a thinning atmosphere. [141]
The presence of methane, a powerful greenhouse gas, in Pluto's atmosphere creates a temperature inversion, with the average temperature of its atmosphere tens of degrees warmer than its surface,[142] though observations by New Horizons have revealed Pluto's upper atmosphere to be far colder than expected (70 K, as opposed to about 100 K). [137] Pluto's atmosphere is divided into roughly 20 regularly spaced haze layers up to 150 km high,[7] thought to be the result of pressure waves created by airflow across Pluto's mountains. [137]
Natural satellites
Main article: Moons of Pluto
Pluto has five known natural satellites. The largest and closest to Pluto is Charon. First identified in 1978 by astronomer James Christy, Charon is the only moon of Pluto that may be in hydrostatic equilibrium. Charon's mass is sufficient to cause the barycenter of the Pluto–Charon system to be outside Pluto. Beyond Charon there are four much smaller circumbinary moons. In order of distance from Pluto they are Styx, Nix, Kerberos, and Hydra. Nix and Hydra were both discovered in 2005,[143] Kerberos was discovered in 2011,[144] and Styx was discovered in 2012. [145] The satellites' orbits are circular (eccentricity < 0.006) and coplanar with Pluto's equator (inclination < 1°),[146][147] and therefore tilted approximately 120° relative to Pluto's orbit. The Plutonian system is highly compact: the five known satellites orbit within the inner 3% of the region where prograde orbits would be stable. [148]
The orbital periods of all Pluto's moons are linked in a system of orbital resonances and near-resonances. [147][149] When precession is accounted for, the orbital periods of Styx, Nix, and Hydra are in an exact 18:22:33 ratio. [147] There is a sequence of approximate ratios, 3:4:5:6, between the periods of Styx, Nix, Kerberos, and Hydra with that of Charon; the ratios become closer to being exact the further out the moons are. [147][150]
The Pluto–Charon system is one of the few in the Solar System whose barycenter lies outside the primary body; the Patroclus–Menoetius system is a smaller example, and the Sun–Jupiter system is the only larger one. [151] The similarity in size of Charon and Pluto has prompted some astronomers to call it a double dwarf planet. [152] The system is also unusual among planetary systems in that each is tidally locked to the other, which means that Pluto and Charon always have the same hemisphere facing each other — a property shared by only one other known system, Eris and Dysnomia. [153] From any position on either body, the other is always at the same position in the sky, or always obscured. [154] This also means that the rotation period of each is equal to the time it takes the entire system to rotate around its barycenter. [98]
Pluto's moons are hypothesized to have been formed by a collision between Pluto and a similar-sized body, early in the history of the Solar System. The collision released material that consolidated into the moons around Pluto. [155]
Quasi-satellite
In 2012, it was calculated that 15810 Arawn could be a quasi-satellite of Pluto, a specific type of co-orbital configuration. [156] According to the calculations, the object would be a quasi-satellite of Pluto for about 350,000 years out of every two-million-year period. [156][157] Measurements made by the New Horizons spacecraft in 2015 made it possible to calculate the orbit of Arawn more accurately,[158] and confirmed the earlier ones. [159] However, it is not agreed upon among astronomers whether Arawn should be classified as a quasi-satellite of Pluto based on its orbital dynamics, since its orbit is primarily controlled by Neptune with only occasional perturbations by Pluto. [160][158][159]
Origin
Further information: Kuiper belt and Nice model
Pluto's origin and identity had long puzzled astronomers. One early hypothesis was that Pluto was an escaped moon of Neptune[161] knocked out of orbit by Neptune's largest moon, Triton. This idea was eventually rejected after dynamical studies showed it to be impossible because Pluto never approaches Neptune in its orbit. [162]
Pluto's true place in the Solar System began to reveal itself only in 1992, when astronomers began to find small icy objects beyond Neptune that were similar to Pluto not only in orbit but also in size and composition. This trans-Neptunian population is thought to be the source of many short-period comets. Pluto is the largest member of the Kuiper belt,[lower-alpha 14] a stable belt of objects located between 30 and 50 AU from the Sun. As of 2011, surveys of the Kuiper belt to magnitude 21 were nearly complete and any remaining Pluto-sized objects are expected to be beyond 100 AU from the Sun. [163] Like other Kuiper-belt objects (KBOs), Pluto shares features with comets; for example, the solar wind is gradually blowing Pluto's surface into space. [164] It has been claimed that if Pluto were placed as near to the Sun as Earth, it would develop a tail, as comets do. [165] This claim has been disputed with the argument that Pluto's escape velocity is too high for this to happen. [166] It has been proposed that Pluto may have formed as a result of the agglomeration of numerous comets and Kuiper-belt objects. [167][168]
Though Pluto is the largest Kuiper belt object discovered,[130] Neptune's moon Triton, which is larger than Pluto, is similar to it both geologically and atmospherically, and is thought to be a captured Kuiper belt object. [169] Eris (see above) is about the same size as Pluto (though more massive) but is not strictly considered a member of the Kuiper belt population. Rather, it is considered a member of a linked population called the scattered disc. [170] | 12 | 4 |
Like other members of the Kuiper belt, Pluto is thought to be a residual planetesimal; a component of the original protoplanetary disc around the Sun that failed to fully coalesce into a full-fledged planet. Most astronomers agree that Pluto owes its position to a sudden migration undergone by Neptune early in the Solar System's formation. As Neptune migrated outward, it approached the objects in the proto-Kuiper belt, setting one in orbit around itself (Triton), locking others into resonances, and knocking others into chaotic orbits. The objects in the scattered disc, a dynamically unstable region overlapping the Kuiper belt, are thought to have been placed in their positions by interactions with Neptune's migrating resonances. [171] A computer model created in 2004 by Alessandro Morbidelli of the Observatoire de la Côte d'Azur in Nice suggested that the migration of Neptune into the Kuiper belt may have been triggered by the formation of a 1:2 resonance between Jupiter and Saturn, which created a gravitational push that propelled both Uranus and Neptune into higher orbits and caused them to switch places, ultimately doubling Neptune's distance from the Sun. The resultant expulsion of objects from the proto-Kuiper belt could also explain the Late Heavy Bombardment 600 million years after the Solar System's formation and the origin of the Jupiter trojans. [172] It is possible that Pluto had a near-circular orbit about 33 AU from the Sun before Neptune's migration perturbed it into a resonant capture. [173] The Nice model requires that there were about a thousand Pluto-sized bodies in the original planetesimal disk, which included Triton and Eris. [172]
Observation and exploration
Observation
Pluto's distance from Earth makes its in-depth study and exploration difficult. Pluto's visual apparent magnitude averages 15.1, brightening to 13.65 at perihelion. [3] To see it, a telescope is required; around 30 cm (12 in) aperture being desirable. [174] It looks star-like and without a visible disk even in large telescopes,[175] because its angular diameter is maximum 0.11". [3]
The earliest maps of Pluto, made in the late 1980s, were brightness maps created from close observations of eclipses by its largest moon, Charon. Observations were made of the change in the total average brightness of the Pluto–Charon system during the eclipses. For example, eclipsing a bright spot on Pluto makes a bigger total brightness change than eclipsing a dark spot. Computer processing of many such observations can be used to create a brightness map. This method can also track changes in brightness over time. [176][177]
Better maps were produced from images taken by the Hubble Space Telescope (HST), which offered higher resolution, and showed considerably more detail,[106] resolving variations several hundred kilometers across, including polar regions and large bright spots. [108] These maps were produced by complex computer processing, which finds the best-fit projected maps for the few pixels of the Hubble images. [178] These remained the most detailed maps of Pluto until the flyby of New Horizons in July 2015, because the two cameras on the HST used for these maps were no longer in service. [178]
Exploration
Main articles: Exploration of Pluto and New Horizons
The New Horizons spacecraft, which flew by Pluto in July 2015, is the first and so far only attempt to explore Pluto directly. Launched in 2006, it captured its first (distant) images of Pluto in late September 2006 during a test of the Long Range Reconnaissance Imager. [179] The images, taken from a distance of approximately 4.2 billion kilometers, confirmed the spacecraft's ability to track distant targets, critical for maneuvering toward Pluto and other Kuiper belt objects. In early 2007 the craft made use of a gravity assist from Jupiter.
New Horizons made its closest approach to Pluto on July 14, 2015, after a 3,462-day journey across the Solar System. Scientific observations of Pluto began five months before the closest approach and continued for at least a month after the encounter. Observations were conducted using a remote sensing package that included imaging instruments and a radio science investigation tool, as well as spectroscopic and other experiments. The scientific goals of New Horizons were to characterize the global geology and morphology of Pluto and its moon Charon, map their surface composition, and analyze Pluto's neutral atmosphere and its escape rate. On October 25, 2016, at 05:48 pm ET, the last bit of data (of a total of 50 billion bits of data; or 6.25 gigabytes) was received from New Horizons from its close encounter with Pluto. [180][181][182][183]
Since the New Horizons flyby, scientists have advocated for an orbiter mission that would return to Pluto to fulfill new science objectives. [184][185][186] They include mapping the surface at 9.1 m (30 ft) per pixel, observations of Pluto's smaller satellites, observations of how Pluto changes as it rotates on its axis, investigations of a possible subsurface ocean, and topographic mapping of Pluto's regions that are covered in long-term darkness due to its axial tilt. The last objective could be accomplished using laser pulses to generate a complete topographic map of Pluto. New Horizons principal investigator Alan Stern has advocated for a Cassini-style orbiter that would launch around 2030 (the 100th anniversary of Pluto's discovery) and use Charon's gravity to adjust its orbit as needed to fulfill science objectives after arriving at the Pluto system. [187] The orbiter could then use Charon's gravity to leave the Pluto system and study more KBOs after all Pluto science objectives are completed. A conceptual study funded by the NASA Innovative Advanced Concepts (NIAC) program describes a fusion-enabled Pluto orbiter and lander based on the Princeton field-reversed configuration reactor. [188][189]
New Horizons imaged all of Pluto's northern hemisphere, and the equatorial regions down to about 30° South. Higher southern latitudes have only been observed, at very low resolution, from Earth. [190] Images from the Hubble Space Telescope in 1996 cover 85% of Pluto and show large albedo features down to about 75° South. [191][192] This is enough to show the extent of the temperate-zone maculae. Later images had slightly better resolution, due to minor improvements in Hubble instrumentation. [193] The equatorial region of the sub-Charon hemisphere of Pluto has only been imaged at low resolution, as New Horizons made its closest approach to the anti-Charon hemisphere. [194]
Some albedo variations in the higher southern latitudes could be detected by New Horizons using Charon-shine (light reflected off Charon). The south polar region seems to be darker than the north polar region, but there is a high-albedo region in the southern hemisphere that may be a regional nitrogen or methane ice deposit. [195]
See also
• How I Killed Pluto and Why It Had It Coming
• List of geological features on Pluto
• Pluto in astrology
• Pluto in fiction
• Stats of planets in the Solar System
Notes
1. This photograph was taken by the Ralph telescope aboard New Horizons on July 14, 2015 from a distance of 35,445 km (22,025 mi)
2. The mean elements here are from the Theory of the Outer Planets (TOP2013) solution by the Institut de mécanique céleste et de calcul des éphémérides (IMCCE). They refer to the standard equinox J2000, the barycenter of the Solar System, and the epoch J2000.
3. Surface area derived from the radius r: $4\pi r^{2}$.
4. Volume v derived from the radius r: $4\pi r^{3}/3$.
5. Surface gravity derived from the mass M, the gravitational constant G and the radius r: $GM/r^{2}$.
6. Escape velocity derived from the mass M, the gravitational constant G and the radius r: ${\sqrt {2GM/r}}$.
7. Based on geometry of minimum and maximum distance from Earth and Pluto radius in the factsheet
8. A French astronomer had suggested the name Pluto for Planet X in 1919, but there is no indication that the Lowell staff knew of this. [28]
9. For example, ⟨♇⟩ (in Unicode: U+2647 ♇ PLUTO) occurs in a table of the planets identified by their symbols in a 2004 article written before the 2006 IAU definition,[32] but not in a graph of planets, dwarf planets and moons from 2016, where only the eight IAU planets are identified by their symbols. [33] (Planetary symbols in general are uncommon in astronomy, and are discouraged by the IAU. )[34]
10. The bident symbol (U+2BD3 ⯓ PLUTO FORM TWO) has seen some astronomical use as well since the IAU decision on dwarf planets, for example in a public-education poster on dwarf planets published by the NASA/JPL Dawn mission in 2015, in which each of the five dwarf planets announced by the IAU receives a symbol. | 12 | 5 |
[36] There are in addition several other symbols for Pluto found in astrological sources,[37] including three accepted by Unicode: , U+2BD4 ⯔ PLUTO FORM THREE, used principally in southern Europe; /, U+2BD6 ⯖ PLUTO FORM FIVE (found in various orientations, showing Pluto's orbit cutting across that of Neptune), used principally in northern Europe; and , U+2BD5 ⯕ PLUTO FORM FOUR, used in Uranian astrology. [38]
11. The equivalence is less close in languages whose phonology differs widely from Greek's, such as Somali Buluuto and Navajo Tłóotoo.
12. The discovery of Charon in 1978 allowed astronomers to accurately calculate the mass of the Plutonian system. But it did not indicate the two bodies' individual masses, which could only be estimated after other moons of Pluto were discovered in late 2005. As a result, because Pluto came to perihelion in 1989, most Pluto perihelion date estimates are based on the Pluto–Charon barycenter. Charon came to perihelion 4 September 1989. The Pluto–Charon barycenter came to perihelion 5 September 1989. Pluto came to perihelion 8 September 1989.
13. Because of the eccentricity of Pluto's orbit, some have theorized that it was once a satellite of Neptune. [94]
14. The dwarf planet Eris is roughly the same size as Pluto, about 2330 km; Eris is 28% more massive than Pluto. Eris is a scattered-disc object, often considered a distinct population from Kuiper-belt objects like Pluto; Pluto is the largest body in the Kuiper belt proper, which excludes the scattered-disc objects.
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Further reading
• Codex Regius (2016), Pluto & Charon, CreateSpace Independent Publishing Platform ISBN 978-1534960749
• Stern, S A and Tholen, D J (1997), Pluto and Charon, University of Arizona Press ISBN 978-0816518401
• Stern, Alan; Grinspoon, David (2018). Chasing New Horizons: Inside the Epic First Mission to Pluto. Picador. ISBN 978-125009896-2.
• Stern, Alan (August 10, 2021). The Pluto System After New Horizons. University of Arizona Press. p. 688. ISBN 978-0816540945.
External links
• New Horizons homepage Archived July 26, 2015, at the Wayback Machine
• Pluto Profile at NASA's Solar System Exploration site
• NASA Pluto factsheet Archived November 19, 2015, at archive.today
• Website of the observatory that discovered Pluto Archived March 2, 2011, at the Wayback Machine
• Earth telescope image of Pluto system
• Keck infrared with AO of Pluto system Archived November 9, 2020, at the Wayback Machine
• Video – Pluto – viewed through the years (GIF) Archived July 26, 2015, at the Wayback Machine (NASA; animation; July 15, 2015).
• Video – Pluto – "FlyThrough" (00:22; MP4) Archived September 29, 2021, at the Wayback Machine (YouTube) Archived December 2, 2020, at the Wayback Machine (NASA; animation; August 31, 2015).
• "A Day on Pluto Video made from July 2015 New Horizon Images" Archived February 23, 2016, at the Wayback Machine Scientific American
• NASA CGI video Archived August 1, 2017, at the Wayback Machine of Pluto flyover (July 14, 2017)
• CGI video Archived October 3, 2020, at the Wayback Machine simulation of rotating Pluto by Seán Doran (see album Archived July 27, 2020, at the Wayback Machine for more)
• Google Pluto 3D Archived August 6, 2020, at the Wayback Machine, interactive map of the dwarf planet
• "Interactive 3D gravity simulation of the Plutonian system". Archived from the original on June 11, 2020.
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Moons of Pluto
The dwarf planet Pluto has five natural satellites. [1] In order of distance from Pluto, they are Charon, Styx, Nix, Kerberos, and Hydra. [2] Charon, the largest, is mutually tidally locked with Pluto, and is massive enough that Pluto and Charon are sometimes considered a binary dwarf planet. [3]
• Top: Pluto's largest moon, Charon, with its dark Mordor Macula
• Middle: Hydra (left) and Nix (right)
• Bottom: Kerberos (left) and Styx (right)
(Images not to scale)
History
The innermost and largest moon, Charon, was discovered by James Christy on 22 June 1978, nearly half a century after Pluto was discovered. This led to a substantial revision in estimates of Pluto's size, which had previously assumed that the observed mass and reflected light of the system were all attributable to Pluto alone.
Two additional moons were imaged by astronomers of the Pluto Companion Search Team preparing for the New Horizons mission and working with the Hubble Space Telescope on 15 May 2005, which received the provisional designations S/2005 P 1 and S/2005 P 2. The International Astronomical Union officially named these moons Nix (or Pluto II, the inner of the two moons, formerly P 2) and Hydra (Pluto III, the outer moon, formerly P 1), on 21 June 2006. [4] Kerberos, announced on 20 July 2011, was discovered while searching for Plutonian rings. The discovery of Styx was announced on 7 July 2012 while looking for potential hazards for New Horizons. [5]
Charon
Main article: Charon (moon)
Charon is about half the diameter of Pluto and is massive enough (nearly one eighth of the mass of Pluto) that the system's barycenter lies between them, approximately 960 km above Pluto's surface. [6][lower-alpha 1] Charon and Pluto are also tidally locked, so that they always present the same face toward each other. The IAU General Assembly in August 2006 considered a proposal that Pluto and Charon be reclassified as a double planet, but the proposal was abandoned. [7] Like Pluto, Charon is a perfect sphere to within measurement uncertainty. [8]
Circumbinary moons
Animation of moons of Pluto around the barycenter of Pluto - Ecliptic plane
Front view
Side view
Pluto · Charon · Styx · Nix · Kerberos · Hydra
The Hubble discovery image of Nix and Hydra
Discovery image of Styx, overlaid with orbits of the satellite system
Pluto's four small circumbinary moons orbit Pluto at two to four times the distance of Charon, ranging from Styx at 42,700 kilometres to Hydra at 64,800 kilometres from the barycenter of the system. They have nearly circular prograde orbits in the same orbital plane as Charon.
All are much smaller than Charon. Nix and Hydra, the two larger, are roughly 42 and 55 kilometers on their longest axis respectively,[9] and Styx and Kerberos are 7 and 12 kilometers respectively. [10][11] All four are irregularly shaped.
Characteristics
The Pluto system is highly compact and largely empty: prograde moons could stably orbit Pluto out to 53% of the Hill radius (the gravitational zone of Pluto's influence) of 6 million km, or out to 69% for retrograde moons. [12] However, only the inner 3% of the region where prograde orbits would be stable is occupied by satellites,[13] and the region from Styx to Hydra is packed so tightly that there is little room for further moons with stable orbits within this region. [14] An intense search conducted by New Horizons confirmed that no moons larger than 4.5 km in diameter exist out to distances up to 180,000 km from Pluto (6% of the stable region for prograde moons), assuming Charon-like albedoes of 0.38 (for smaller distances, this threshold is still smaller). [15]
The relative masses of Pluto's moons. Charon dominates the system. Nix and Hydra are barely visible and Styx and Kerberos are invisible at this scale.
An oblique schematic view of the Pluto–Charon system showing that Pluto orbits a point outside itself. Also visible is the mutual tidal locking between the two bodies.
The orbits of the moons are confirmed to be circular and coplanar, with inclinations differing less than 0.4° and eccentricities less than 0.005. [16]
The discovery of Nix and Hydra suggested that Pluto could have a ring system. Small-body impacts could eject debris off of the small moons which can form into a ring system. However, data from a deep-optical survey by the Advanced Camera for Surveys on the Hubble Space Telescope, by occultation studies,[17] and later by New Horizons, suggest that no ring system is present.
Resonances
Styx, Nix, and Hydra are thought to be in a 3-body Laplace orbital resonance with orbital periods in a ratio of 18:22:33. [18][19] The ratios should be exact when orbital precession is taken into account. Nix and Hydra are in a simple 2:3 resonance. [lower-alpha 2][18][20] Styx and Nix are in an 9:11 resonance, while the resonance between Styx and Hydra has a ratio of 6:11. [lower-alpha 3] The Laplace resonance also means that ratios of synodic periods are then such that there are 5 Styx–Hydra conjunctions and 3 Nix–Hydra conjunctions for every 2 conjunctions of Styx and Nix. [lower-alpha 4][18] If $\lambda $ denotes the mean longitude and $\Phi $ the libration angle, then the resonance can be formulated as $\Phi =3\lambda _{\rm {Styx}}-5\lambda _{\rm {Nix}}+2\lambda _{\rm {Hydra}}=180^{\circ }$. As with the Laplace resonance of the Galilean satellites of Jupiter, triple conjunctions never occur. $\Phi $ librates about 180° with an amplitude of at least 10°. [18]
All of the outer circumbinary moons are also close to mean motion resonance with the Charon–Pluto orbital period. Styx, Nix, Kerberos, and Hydra are in a 1:3:4:5:6 sequence of near resonances, with Styx approximately 5.4% from its resonance, Nix approximately 2.7%, Kerberos approximately 0.6%, and Hydra approximately 0.3%. [21] It may be that these orbits originated as forced resonances when Charon was tidally boosted into its current synchronous orbit, and then released from resonance as Charon's orbital eccentricity was tidally damped. The Pluto–Charon pair creates strong tidal forces, with the gravitational field at the outer moons varying by 15% peak to peak.
However, it was calculated that a resonance with Charon could boost either Nix or Hydra into its current orbit, but not both: boosting Hydra would have required a near-zero Charonian eccentricity of 0.024, whereas boosting Nix would have required a larger eccentricity of at least 0.05. This suggests that Nix and Hydra were instead captured material, formed around Pluto–Charon, and migrated inward until they were trapped in resonance with Charon. [22] The existence of Kerberos and Styx may support this idea.
Configurations of Hydra (blue), Nix (red) and Styx (black) over one quarter of the cycle of their mutual orbital resonance. Movements are counterclockwise and orbits completed are tallied at upper right of diagrams (click on image to see the complete cycle).
Rotation
Prior to the New Horizons mission, Nix, Hydra, Styx, and Kerberos were predicted to rotate chaotically or tumble. [18][23]
However, New Horizons imaging found that they had not tidally spun down to near a spin synchronous state where chaotic rotation or tumbling would be expected. [24][25] New Horizons imaging found that all 4 moons were at high obliquity. [24] Either they were born that way, or they were tipped by a spin precession resonance. [25] Styx may be experiencing intermittent and chaotic obliquity variations.
Mark R. Showalter had speculated that, "Nix can flip its entire pole. It could actually be possible to spend a day on Nix in which the sun rises in the east and sets in the north. It is almost random-looking in the way it rotates. "[26] Only one other moon, Saturn's moon Hyperion, is known to tumble,[27] though it is likely that Haumea's moons do so as well. [28]
Origin
It is suspected that Pluto's satellite system was created by a massive collision, similar to the Theia impact thought to have created the Moon. [29][30] In both cases, the high angular momenta of the moons can only be explained by such a scenario. | 13 | 0 |
The nearly circular orbits of the smaller moons suggests that they were also formed in this collision, rather than being captured Kuiper Belt objects. This and their near orbital resonances with Charon (see below) suggest that they formed closer to Pluto than they are at present and migrated outward as Charon reached its current orbit. Their grey color is different from that of Pluto, one of the reddest bodies in the Solar System. This is thought to be due to a loss of volatiles during the impact or subsequent coalescence, leaving the surfaces of the moons dominated by water ice. However, such an impact should have created additional debris (more moons), yet no moons or rings were discovered by New Horizons, ruling out any more moons of significant size orbiting Pluto. [1]
List
Pluto's moons are listed here by orbital period, from shortest to longest. Charon, which is massive enough to have collapsed into a spheroid under its own gravitation, is highlighted in light purple. As the system barycenter lies far above Pluto's surface, its barycentric orbital elements have been included as well. [18][31] All elements are with respect to the Pluto-Charon barycenter. [18] The mean separation distance between the centers of Pluto and Charon is 19,596 km. [32]
Label
[lower-alpha 5] Name
(pronunciation) Named after[34] Image Diameter
(km) Mass (×1019 kg)[35] Semi-major
axis (km) Orbital period
(days) Orbital resonance
(relative to Charon) Eccentricity Inclination (°)
(to Pluto's equator) Visual
magnitude (mean) Discovery
year
Pluto/ˈpluːtoʊ/Pluto, Roman god of the underworld2376.6±3.21305±72035[32]6.387231 : 10.0022[lower-alpha 6]0.00115.11930
ICharon/ˈʃærən/,[lower-alpha 7]
/ˈkɛərən/ Charon, ferryman of the underworld in Greek mythology1212±1158.7±1.517536±36.387231 : 10.0022[lower-alpha 6]0.08016.81978
VStyx/ˈstɪks/The mythical river Styx and its eponymous goddess16 × 9 × 8[36]0.0007542656±7820.161551 : 3.160.005790.81±0.16272012
IINix/ˈnɪks/Egyptian spelling of Nyx, goddess of the night in Greek mythology49.8 × 33.2 × 31.1 [37]0.005±0.00448694±324.854631 : 3.890.002040.133±0.00823.72005
IVKerberos/ˈkɜːrbərəs, -ɒs/Greek spelling of Cerberus, the many-headed dog who guards the Greek underworld19 × 10 × 9[36]0.0016±0.000957783±1932.167561 : 5.040.003280.389±0.037262011
IIIHydra/ˈhaɪdrə/The Hydra, the many-headed serpent who guards the Greek underworld50.9 × 36.1 × 30.9 [37]0.005±0.00464738±338.201771 : 5.980.005860.242±0.00523.32005
Scale model of the Pluto system
• Pluto and its five moons, including the location of the system's barycenter. Sizes and distances of the bodies are to scale.
Mutual events
Transits occur when one of Pluto's moons passes between Pluto and the Sun. This occurs when one of the satellites' orbital nodes (the points where their orbits cross Pluto's ecliptic) lines up with Pluto and the Sun. This can only occur at two points in Pluto's orbit; coincidentally, these points are near Pluto's perihelion and aphelion. Occultations occur when Pluto passes in front of and blocks one of Pluto's satellites.
Charon has an angular diameter of 4 degrees of arc as seen from the surface of Pluto; the Sun appears much smaller, only 39 to 65 arcseconds. By comparison, the Moon as viewed from Earth has an angular diameter of only 31 minutes of arc, or just over half a degree of arc. Therefore, Charon would appear to have eight times the diameter, or 25 times the area of the Moon; this is due to Charon's proximity to Pluto rather than size, as despite having just over one-third of a Lunar radius, Earth's Moon is 20 times more distant from Earth's surface as Charon is from Pluto's. This proximity further ensures that a large proportion of Pluto's surface can experience an eclipse. Because Pluto always presents the same face towards Charon due to tidal locking, only the Charon-facing hemisphere experiences solar eclipses by Charon.
The smaller moons can cast shadows elsewhere. The angular diameters of the four smaller moons (as seen from Pluto) are uncertain. Nix's is 3–9 minutes of arc and Hydra's is 2–7 minutes. These are much larger than the Sun's angular diameter, so total solar eclipses are caused by these moons.
Eclipses by Styx and Kerberos are more difficult to estimate, as both moons are very irregular, with angular dimensions of 76.9 x 38.5 to 77.8 x 38.9 arcseconds for Styx, and 67.6 x 32.0 to 68.0 x 32.2 for Kerberos. As such, Styx has no annular eclipses, its widest axis being more than 10 arcseconds larger than the Sun at its largest. However, Kerberos, although slightly larger, cannot make total eclipses as its largest minor axis is a mere 32 arcseconds. Eclipses by Kerberos and Styx will entirely consist of partial and hybrid eclipses, with total eclipses being extremely rare.
The next period of mutual events due to Charon will begin in October 2103, peak in 2110, and end in January 2117. During this period, solar eclipses will occur once each Plutonian day, with a maximum duration of 90 minutes. [38][39]
Exploration
The Pluto system was visited by the New Horizons spacecraft in July 2015. Images with resolutions of up to 330 meters per pixel were returned of Nix and up to 1.1 kilometers per pixel of Hydra. Lower-resolution images were returned of Styx and Kerberos. [40]
Notes
1. "P1P2_motion.avi". Archived from the original (AVI) on 4 November 2005. and barycenter for animations
2. The ratio of 18:22:33 in the 3-body resonance corresponds to a 2-body resonance with ratio 2:3 between Hydra and Nix.
3. The ratio of 18:22:33 in the 3-body resonance corresponds to a 2-body resonance with ratio 9:11 between Styx and Nix. In analogy, the ratio of 18:22:33 in the 3-body resonance corresponds to a 2-body resonance with ratio 6:11 between Styx and Hydra.
4. This is calculated as follows: for every $1$ orbit of Hydra there are ${\frac {33}{22}}={\frac {3}{2}}$ orbits of Nix and ${\frac {33}{18}}={\frac {11}{6}}$ orbits of Styx. The conjunctions then occur at a relative rate of ${\frac {11}{6}}-1={\frac {5}{6}}$ for Styx-Hydra, ${\frac {3}{2}}-1={\frac {1}{2}}$ for Nix-Hydra and ${\frac {11}{6}}-{\frac {3}{2}}={\frac {1}{3}}$ for Styx-Nix. Multiplying all three rates by $6$ (to make them integers) yields that there are $5$ Styx-Hydra conjunctions and $3$ Nix-Hydra conjunctions for every $2$ Styx-Nix conjunctions.
5. Label refers to the Roman numerals attributed to each moon in order of their discovery. [33]
6. Orbital eccentricity and inclination of Pluto and Charon are equal because they refer to the same two-body problem (the gravitational influence of the smaller satellites is neglected here).
7. Many astronomers use this, Christy's pronunciation, rather than the classical /ˈkɛərɒn/, but both are considered to be acceptable.
References
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31. | 13 | 2 |
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36. "Special Session: Planet 9 from Outer Space - Pluto Geology and Geochemistry". YouTube. Lunar and Planetary Institute. 25 March 2016. Archived from the original on 21 December 2021. Retrieved 27 May 2019.
37. Verbiscer, A. J.; Porter, S. B.; Buratti, B. J.; Weaver, H. A.; Spencer, J. R.; Showalter, M. R.; Buie, M. W.; Hofgartner, J. D.; Hicks, M. D.; Ennico-Smith, K.; Olkin, C. B.; Stern, S. A.; Young, L. A.; Cheng, A. (2018). "Phase Curves of Nix and Hydra from the New Horizons Imaging Cameras". The Astrophysical Journal. 852 (2): L35. Bibcode:2018ApJ...852L..35V. doi:10.3847/2041-8213/aaa486.
38. "Start of Eclipse". JPL Solar System Simulator. 12 December 1987. Archived from the original on 24 March 2017. Retrieved 29 July 2014. (Pluto as seen from the Sun during mid-eclipse)
39. "End of Eclipse". JPL Solar System Simulator. 12 December 1987. Archived from the original on 24 March 2017. Retrieved 29 July 2014.
40. "New Horizons flyby timeline". Archived from the original on 15 July 2015. Retrieved 25 July 2015.
Sources
• Stern, S. A.; Weaver, H. A.; Steffl, A. J.; Mutchler, M. J.; Merline, W. J.; Buie, M. W.; Young, E. F.; Young, L. A.; Spencer, J. R. (2005). "Characteristics and Origin of the Quadruple System at Pluto". arXiv:astro-ph/0512599.
• Steffl, A. J.; Mutchler, M. J.; Weaver, H. A.; Stern, S. A.; Durda, D. D.; Terrell, D.; Merline, W. J.; Young, L. A.; Young, E. F.; Buie, M. W.; Spencer, J. R. (2006). "New Constraints on Additional Satellites of the Pluto System". The Astronomical Journal. 132 (2): 614–619. arXiv:astro-ph/0511837. Bibcode:2006AJ....132..614S. doi:10.1086/505424. S2CID 10547358.
• Buie, Marc W.; Grundy, William M.; Young, Eliot F.; Young, Leslie A.; Stern, S. Alan (2006). "Orbits and Photometry of Pluto's Satellites: Charon, S/2005 P1, and S/2005 P2". The Astronomical Journal. 132 (1): 290–298. arXiv:astro-ph/0512491. Bibcode:2006AJ....132..290B. doi:10.1086/504422. S2CID 119386667.
• Brozović, Marina; Showalter, Mark R.; Jacobson, Robert A.; Buie, Marc W. (2015). "The orbits and masses of satellites of Pluto". Icarus. 246: 317–329. Bibcode:2015Icar..246..317B. doi:10.1016/j.icarus.2014.03.015.
• Codex Regius (2016), Pluto & Charon, CreateSpace Independent Publishing Platform ISBN 978-1534960749
• IAU Circular No. 8625, describing the discovery of 2005 P1 and P2
• IAU Circular No. 8686, reporting a more neutral color for 2005 P2
• IAU Circular No. 8723 announcing the names of Nix and Hydra
• Background Information Regarding Our Two Newly Discovered Satellites of Pluto – The website of the discoverers of Nix and Hydra
External links
Wikimedia Commons has media related to Moons of Pluto.
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(143651) 2003 QO104
(143651) 2003 QO104, provisional designation 2003 QO104, is a stony asteroid, slow rotator and suspected tumbler on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Amor and Apollo group, respectively. It was discovered on 31 August 2003, by astronomers of the Near-Earth Asteroid Tracking program at the Haleakala Observatory in Hawaii, United States. [1] The Q-type asteroid has a rotation period of 114.4 hours and possibly an elongated shape. It measures approximately 2.3 kilometers (1.4 miles) in diameter and belongs the largest potentially hazardous asteroids known to exist. [14]
(143651) 2003 QO104
Discovery[1]
Discovered byNEAT
Discovery siteHaleakala Obs.
Discovery date31 August 2003
Designations
MPC designation
(143651) 2003 QO104
Alternative designations
2003 QO104
Minor planet category
NEO · PHA[1][2]
Apollo[2] · Amor[1]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc36.55 yr (13,349 d)
Aphelion3.2551 AU
Perihelion1.0151 AU
Semi-major axis
2.1351 AU
Eccentricity0.5246
Orbital period (sidereal)
3.12 yr (1,140 d)
Mean anomaly
297.32°
Mean motion
0° 18m 57.24s / day
Inclination11.608°
Longitude of ascending node
58.224°
Argument of perihelion
183.53°
Earth MOID0.0042 AU (1.6362 LD)
Physical characteristics
Mean diameter
1.88 km (calculated)[3]
2.29±0.54 km[4]
2.31 km[5]
Synodic rotation period
113.3±0.1 h[6]
114±3 h[7]
114.4±0.1 h[8][lower-alpha 1]
Geometric albedo
0.13[5]
0.137±0.140[4]
0.14±0.12[9]
0.20 (assumed)[3]
Spectral type
Q[10] · S (assumed)[3]
B–V = 0.903±0.008[11]
V–R = 0.454±0.011[11]
V–I = 0.797±0.019[11]
B–V = 0.880±0.020[12]
V–R = 0.450±0.020[12]
Absolute magnitude (H)
16.0[2][3][5]
16.48±0.43[13]
Orbit and classification
2003 QO104 is a member of the Apollo group of asteroids, which are Earth-crossing asteroids. They are the largest group of near-Earth objects with approximately 10 thousand known members. As it just grazes the orbit of Earth, the Minor Planet Center (MPC), groups it to the non-Earth crossing Amor asteroids. [1]
It orbits the Sun at a distance of 1.015–3.3 AU once every 3 years and 1 month (1,140 days; semi-major axis of 2.14 AU). Its orbit has an eccentricity of 0.52 and an inclination of 12° with respect to the ecliptic. [2] The body's observation arc begins with a precovery taken at the Siding Spring Observatory on in July 1981, more than 18 years prior to its official discovery observation at Haleakala. [1]
Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0042 AU (628,000 km; 390,000 mi), which corresponds to 1.6 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. [2] On the Torino Scale, this object was rated level 1 in early October 2003,[15] and removed on 13 October 2003. [16]
On 18 May 1985, it passed Earth at a nominal distance of 0.00709 AU (2.76 LD) which translates into 1,060,648 km (659,000 mi) and made another approach in June 2009 at a much larger distance of 37 LD. [17] In 2034, 2037 and 2062, it will pass Earth at a distance of 0.18 AU, 0.44 AU and 0.045 AU, respectively. It frequently approaches Jupiter at 1.7–2.0 AU as well. [17]
History of close approaches of large near-Earth objects since 1908 (A)
PHA Date Approach distance (lunar dist.) Abs.
mag
(H) Diameter (C)
(m) Ref (D)
Nomi-
nal(B) Mini-
mum Maxi-
mum
(33342) 1998 WT241908-12-163.5423.5373.54717.9556–1795data
(458732) 2011 MD51918-09-170.9110.9090.91317.9556–1795data
(7482) 1994 PC11933-01-172.9272.9272.92816.8749–1357data
69230 Hermes1937-10-301.9261.9261.92717.5668–2158data
69230 Hermes1942-04-261.6511.6511.65117.5668–2158data
(137108) 1999 AN101946-08-072.4322.4292.43517.9556–1795data
(33342) 1998 WT241956-12-163.5233.5233.52317.9556–1795data
(163243) 2002 FB31961-04-124.9034.9004.90616.41669–1695data
(192642) 1999 RD321969-08-273.6273.6253.63016.31161–3750data
(143651) 2003 QO1041981-05-182.7612.7602.76116.01333–4306data
2017 CH11992-06-054.6913.3916.03717.9556–1795data
(170086) 2002 XR141995-06-244.2594.2594.26018.0531–1714data
(33342) 1998 WT242001-12-164.8594.8594.85917.9556–1795data
4179 Toutatis2004-09-294.0314.0314.03115.32440–2450data
2014 JO252017-04-194.5734.5734.57317.8582–1879data
(137108) 1999 AN102027-08-071.0141.0101.01917.9556–1795data
(35396) 1997 XF112028-10-262.4172.4172.41816.9881–2845data
(154276) 2002 SY502071-10-303.4153.4123.41817.6714–1406data
(164121) 2003 YT12073-04-294.4094.4094.40916.21167–2267data
(385343) 2002 LV2076-08-044.1844.1834.18516.61011–3266data
(52768) 1998 OR22079-04-164.6114.6114.61215.81462–4721data
(33342) 1998 WT242099-12-184.9194.9194.91917.9556–1795data
(85182) 1991 AQ2130-01-274.1404.1394.14117.11100data
314082 Dryope2186-07-163.7092.9964.78617.5668–2158data
(137126) 1999 CF92192-08-214.9704.9674.97318.0531–1714data
(290772) 2005 VC2198-05-051.9511.7912.13417.6638–2061data | 14 | 0 |
(A) List includes near-Earth approaches of less than 5 lunar distances (LD) of objects with H brighter than 18.
(B) Nominal geocentric distance from the Earth's center to the object's center (Earth radius≈0.017 LD).
(C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
(D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
(E) Color codes: unobserved at close approach observed during close approach upcoming approaches
Physical characteristics
2003 QO104 has been characterized as an uncommon Q-type asteroid,[10] that falls into the larger stony S-complex. [3]
Slow rotator and tumbler
Several rotational lightcurve of this asteroid were obtained from photometric observations during its close approach to the Earth in 2009. [6][7][8] Analysis of the best-rated lightcurve – obtained by Brian Warner at his Palmer Divide Observatory in collaboration with Robert Stephens and Albino Carbognani – gave a well-defined rotation period of 114.4 hours with a high brightness amplitude of 1.60 magnitude (U=3), which is indicative of an elongated shape. [8][lower-alpha 1] With a period of more than 100 hours, 2003 QO104 is a slow rotator as most asteroids typically rotate every 2 to 20 hours once around their axis. The asteroid also shows several characteristics of a non-principal axis-rotation, which is commonly known as tumbling. [7][8]
This asteroid has also been studied by radar at the Goldstone and Arecibo observatories by Lance Benner and Mike Nolan. [8][lower-alpha 2]
Diameter and albedo
According to post-cryogenic observations made by the Spitzer Space Telescope during the ExploreNEOs survey, this asteroid measures 2.29 and 2.31 kilometers in diameter and its surface has an albedo between 0.13 and 0.14,[4][5][9] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 1.88 kilometers based on an absolute magnitude of 16.0. [3]
Naming
This minor planet was numbered by the MPC on 5 December 2006 (M.P.C. 58189). [18] As of 2018, it has not been named. [1]
Notes
1. Lightcurve plot of (143651) 2003 QO104 by Brian Warner at the Palmer Divide Observatory. Rotation period 114.4±0.1 hours and a brightness amplitude of 1.60±0.03 mag. Quality code of 3. Summary figures at the LCDB and the observatory's website
2. Radiometric observations of (143651) 2003 QO104 at the Arecibo Observatory by Mike Nolan R2421 in May 2009, and at the Goldstone Observatory by Lance Benner Planning in June 2009
References
1. "143651 (2003 QO104)". Minor Planet Center. Retrieved 20 April 2018.
2. "JPL Small-Body Database Browser: 143651 (2003 QO104)" (2018-01-26 last obs.). Jet Propulsion Laboratory. Retrieved 20 April 2018.
3. "LCDB Data for (143651)". Asteroid Lightcurve Database (LCDB). Retrieved 20 April 2018.
4. Mueller, Michael; Delbo', M.; Hora, J. L.; Trilling, D. E.; Bhattacharya, B.; Bottke, W. F.; et al. (April 2011). "ExploreNEOs. III. Physical Characterization of 65 Potential Spacecraft Target Asteroids". The Astronomical Journal. 141 (4): 9. Bibcode:2011AJ....141..109M. doi:10.1088/0004-6256/141/4/109. S2CID 44827674.
5. Trilling, D. E.; Mueller, M.; Hora, J. L.; Harris, A. W.; Bhattacharya, B.; Bottke, W. F.; et al. (September 2010). "ExploreNEOs. I. Description and First Results from the Warm Spitzer Near-Earth Object Survey" (PDF). The Astronomical Journal. 140 (3): 770–784. Bibcode:2010AJ....140..770T. doi:10.1088/0004-6256/140/3/770. S2CID 3006566.
6. Birtwhistle, Peter (October 2009). "Lightcurves for Five Close Approach Asteroids". The Minor Planet Bulletin. 36 (4): 186–187. Bibcode:2009MPBu...36..186B. ISSN 1052-8091.
7. Koehn, Bruce W.; Bowell, Edward G.; Skiff, Brian A.; Sanborn, Jason J.; McLelland, Kyle P.; Pravec, Petr; et al. (October 2014). "Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) - 2009 January through 2009 June". The Minor Planet Bulletin. 41 (4): 286–300. Bibcode:2014MPBu...41..286K. ISSN 1052-8091.
8. Warner, Brian D.; Stephens, Robert D.; Carbognani, Albino (October 2009). "Analysis of the Slow Rotator (143651) 2003 QO104". The Minor Planet Bulletin. 36 (4): 179–180. Bibcode:2009MPBu...36..179W. ISSN 1052-8091.
9. Thomas, C. A.; Trilling, D. E.; Emery, J. P.; Mueller, M.; Hora, J. L.; Benner, L. A. M.; et al. (September 2011). "ExploreNEOs. V. Average Albedo by Taxonomic Complex in the Near-Earth Asteroid Population". The Astronomical Journal. 142 (3): 12. Bibcode:2011AJ....142...85T. doi:10.1088/0004-6256/142/3/85.
10. Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbó, Marco; Hora, Joseph L.; Mueller, Michael (January 2014). "Physical characterization of Warm Spitzer-observed near-Earth objects". Icarus. 228: 217–246. arXiv:1310.2000. Bibcode:2014Icar..228..217T. doi:10.1016/j.icarus.2013.10.004. S2CID 119278697.
11. Ye, Q.-z. (February 2011). "BVRI Photometry of 53 Unusual Asteroids". The Astronomical Journal. 141 (2): 8. arXiv:1011.0133. Bibcode:2011AJ....141...32Y. doi:10.1088/0004-6256/141/2/32. S2CID 119307210.
12. Betzler, Alberto S.; Noaves, Alberto B.; Santos, Antonio C. P.; Sobral, Edvaldo G. (July 2010). "Photometric Observations of the Near-Earth Asteroids 1999 AP10 2000 TO64, 2000 UJ1, 2000 XK44, 2001 MZ7, 2003 QO104, 2005 RQ6, 2005 WJ56, and 2009 UN3". The Minor Planet Bulletin. 37 (3): 95–97. Bibcode:2010MPBu...37...95B. ISSN 1052-8091.
13. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339.
14. "List of the Potentially Hazardous Asteroids (PHAs)". Minor Planet Center. Retrieved 20 April 2018.
15. "Major News about Minor Objects (2003 QO104)". hohmanntransfer. 27 December 2003. Retrieved 20 April 2018.
16. "NEOs Removed from Impact Risks Tables". Near Earth Object Program. NASA. | 14 | 1 |
Archived from the original on 2 June 2002. Retrieved 20 April 2018.
17. "JPL Small-Body Database Browser: 143651 (2003 QO104)". Jet Propulsion Laboratory. Retrieved 20 April 2018.
18. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 April 2018.
External links
• PHA Close Approaches To The Earth, Minor Planet Center
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Retracted lightcurve of (143651) 2003 QO104, René Roy, May 2009, published by Geneva Obs., Raoul Behrend
• List Of Amor Minor Planets (by designation), Minor Planet Center
• (143651) 2003 QO104 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (143651) 2003 QO104 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary
• (143651) 2003 QO104 at the JPL Small-Body Database
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• Active
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• Asteroid belt
• Family
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• Near-Earth
• Spectral types
Distant minor planet
• Centaur
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• Detached
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Authority control databases
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• MPC | 14 | 2 |
(144908) 2004 YH32
(144908) 2004 YH32, provisional designation 2004 YH32, is a centaur and damocloid orbiting the Sun with a very high inclination of almost 80°. [3] It was discovered on 18 December 2004 by the Siding Spring Survey at the Siding Spring Observatory in Australia. The critical and unusual object measures approximately 12 kilometers (7.5 miles) in diameter. [1]
(144908) 2004 YH32
Discovery[1][2]
Discovered bySSS
Discovery siteSiding Spring Obs.
Discovery date18 December 2004
Designations
MPC designation
(144908) 2004 YH32
Alternative designations
2004 YH32
Minor planet category
centaur[3] · damocloid[4]
unusual[5] · distant[1]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 3
Observation arc2.08 yr (758 d)
Aphelion12.777 AU
Perihelion3.5507 AU
Semi-major axis
8.1641 AU
Eccentricity0.5651
Orbital period (sidereal)
23.33 yr (8,520 d)
Mean anomaly
212.33°
Mean motion
0° 2m 32.28s / day
Inclination78.978°
Longitude of ascending node
47.727°
Argument of perihelion
348.73°
TJupiter1.0330
Physical characteristics
Mean diameter
12 km[4]
Geometric albedo
0.09 (assumed)[4]
Absolute magnitude (H)
12.9[1][3]
Orbit and classification
It orbits the Sun at a distance of 3.6–12.8 AU once every 23 years and 4 months (8,520 days; semi-major axis of 8.16 AU). Its orbit has an eccentricity of 0.57 and an inclination of 79° with respect to the ecliptic. [3] The body's observation arc begins with its official discovery observation at the Siding Spring Observatory in December 2004. [1]
Physical characteristics
Johnston's Archive assumes a standard albedo of 0.09 and calculates a diameter of 12 kilometers based on an absolute magnitude of 12.9. [4]
References
1. "144908 (2004 YH32)". Minor Planet Center. Retrieved 20 November 2018.
2. "MPEC 2004-Y61 : 2004 YH32". Minor Planet Center. 25 December 2004. Retrieved 20 November 2018.
3. "JPL Small-Body Database Browser: 144908 (2004 YH32)" (2007-01-15 last obs.). Jet Propulsion Laboratory. Retrieved 20 November 2018.
4. Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 17 January 2018.
5. "List Of Other Unusual Objects". Minor Planet Center. 14 November 2018. Retrieved 20 November 2018.
External links
• MPEC 2007-A22 : CRITICAL-LIST MINOR PLANETS (2007 JAN. 20.0 TT), Minor Planet Center
• (144908) 2004 YH32, Small Bodies Data Ferret
• (144908) 2004 YH32 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (144908) 2004 YH32 at the JPL Small-Body Database
Minor planets navigator
• 144907 Whitehorne
• (144908) 2004 YH32
Small Solar System bodies
Minor planets
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• MPC | 15 | 0 |
(154276) 2002 SY50
(154276) 2002 SY50, provisional designation 2002 SY50, is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 1.1 kilometers (0.7 miles) in diameter. It was discovered on 30 September 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [1] The K-type asteroid has a rotation period of 4.8 hours. [3][lower-alpha 1] It will make a close encounter with Earth on 30 October 2071. [6]
(154276) 2002 SY50
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date30 September 2002
Designations
MPC designation
(154276) 2002 SY50
Alternative designations
2002 SY50
Minor planet category
Apollo · NEO · PHA[1][2]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc11.78 yr (4,304 d)
Aphelion2.8793 AU
Perihelion0.5297 AU
Semi-major axis
1.7045 AU
Eccentricity0.6892
Orbital period (sidereal)
2.23 yr (813 d)
Mean anomaly
305.15°
Mean motion
0° 26m 34.44s / day
Inclination8.7443°
Longitude of ascending node
34.298°
Argument of perihelion
99.395°
Earth MOID0.0027 AU (1.0519 LD)
Physical characteristics
Mean diameter
0.897 km (calculated)[3]
1.060±0.346 km[4]
Synodic rotation period
4.823 h[lower-alpha 1]
Geometric albedo
0.143±0.173[4]
0.20 (assumed)[3]
Spectral type
K[5] · S (assumed)[3]
Absolute magnitude (H)
17.00[5]
17.6[2][3][4]
Orbit and classification
2002 SY50 is a member of the Earth-crossing group of Apollo asteroids, the largest group of near-Earth objects with approximately 10 thousand known members. [1][2]
It orbits the Sun at a distance of 0.53–2.88 AU once every 2 years and 3 months (813 days; semi-major axis of 1.7 AU). Its orbit has an eccentricity of 0.69 and an inclination of 9° with respect to the ecliptic. [2] Due to its large aphelion of 2.88 AU, it also crosses the orbit of Mars at 1.66 AU. [2] The body's observation arc begins one month prior to its official discovery observation with its first observation by the NEAT program at Palomar Observatory in August 2002. [1]
Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0027 AU (404,000 km; 251,000 mi), which corresponds to 1.05 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. [2]
In November 1933, it approached Earth at a nominal distance of 0.098 AU (38 LD), and in November 2002 at 0.084 AU (33 LD). Its closest near-Earth encounter is predicted to occur on 30 October 2071, at a distance of 0.0088 AU (3.4 LD) only (see table). [6]
History of close approaches of large near-Earth objects since 1908 (A)
PHA Date Approach distance (lunar dist.) Abs.
mag
(H) Diameter (C)
(m) Ref (D)
Nomi-
nal(B) Mini-
mum Maxi-
mum
(33342) 1998 WT241908-12-163.5423.5373.54717.9556–1795data
(458732) 2011 MD51918-09-170.9110.9090.91317.9556–1795data
(7482) 1994 PC11933-01-172.9272.9272.92816.8749–1357data
69230 Hermes1937-10-301.9261.9261.92717.5668–2158data
69230 Hermes1942-04-261.6511.6511.65117.5668–2158data
(137108) 1999 AN101946-08-072.4322.4292.43517.9556–1795data
(33342) 1998 WT241956-12-163.5233.5233.52317.9556–1795data
(163243) 2002 FB31961-04-124.9034.9004.90616.41669–1695data
(192642) 1999 RD321969-08-273.6273.6253.63016.31161–3750data
(143651) 2003 QO1041981-05-182.7612.7602.76116.01333–4306data
2017 CH11992-06-054.6913.3916.03717.9556–1795data
(170086) 2002 XR141995-06-244.2594.2594.26018.0531–1714data
(33342) 1998 WT242001-12-164.8594.8594.85917.9556–1795data
4179 Toutatis2004-09-294.0314.0314.03115.32440–2450data
2014 JO252017-04-194.5734.5734.57317.8582–1879data
(137108) 1999 AN102027-08-071.0141.0101.01917.9556–1795data
(35396) 1997 XF112028-10-262.4172.4172.41816.9881–2845data
(154276) 2002 SY502071-10-303.4153.4123.41817.6714–1406data
(164121) 2003 YT12073-04-294.4094.4094.40916.21167–2267data
(385343) 2002 LV2076-08-044.1844.1834.18516.61011–3266data
(52768) 1998 OR22079-04-164.6114.6114.61215.81462–4721data
(33342) 1998 WT242099-12-184.9194.9194.91917.9556–1795data
(85182) 1991 AQ2130-01-274.1404.1394.14117.11100data
314082 Dryope2186-07-163.7092.9964.78617.5668–2158data
(137126) 1999 CF92192-08-214.9704.9674.97318.0531–1714data
(290772) 2005 VC2198-05-051.9511.7912.13417.6638–2061data
(A) List includes near-Earth approaches of less than 5 lunar distances (LD) of objects with H brighter than 18.
(B) Nominal geocentric distance from the Earth's center to the object's center (Earth radius≈0.017 LD).
(C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
(D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
(E) Color codes: unobserved at close approach observed during close approach upcoming approaches
Physical characteristics
Photometry by the Sloan Digital Sky Survey has characterized 2002 SY50 as an uncommon K-type asteroid,[5] which is typically seen among members of the Eos family in the asteroid belt. [7]: 23
Rotation period
In October 2002, a rotational lightcurve of this asteroid was obtained from photometric observations by Italian astronomer Gianluca Masi at the Campo Catino Astronomical Observatory (468). | 16 | 0 |
Lightcurve analysis gave a well-defined rotation period of 4.823 hours with a brightness amplitude of 0.52 magnitude (U=3). [lower-alpha 1]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures 1.06 kilometers in diameter and its surface has an albedo of 0.14,[4] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 0.897 kilometers based on an absolute magnitude of 17.6. [3]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 2 April 2007 (M.P.C. 59337). [8] As of 2018, it has not been named. [1]
Notes
1. Lightcurve plot of (154276) 2002 SY50 from October 2002. Rotation period 4.823 hours with a brightness amplitude of 0.52 mag. Quality code of 3. Summary figures at the LCDB.
References
1. "154276 (2002 SY50)". Minor Planet Center. Retrieved 20 April 2018.
2. "JPL Small-Body Database Browser: 154276 (2002 SY50)" (2014-06-07 last obs.). Jet Propulsion Laboratory. Retrieved 20 April 2018.
3. "LCDB Data for (154276)". Asteroid Lightcurve Database (LCDB). Retrieved 20 April 2018.
4. Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. S2CID 9341381.
5. Carry, B.; Solano, E.; Eggl, S.; DeMeo, F. E. (April 2016). "Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry". Icarus. 268: 340–354. arXiv:1601.02087. Bibcode:2016Icar..268..340C. doi:10.1016/j.icarus.2015.12.047. S2CID 119258489.
6. "Close-Approach Data, JPL Small-Body Database Browser: 154276 (2002 SY50)". Jet Propulsion Laboratory. Retrieved 20 April 2018.
7. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. S2CID 119280014.
8. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 April 2018.
External links
• List of the Potentially Hazardous Asteroids (PHAs), Minor Planet Center
• PHA Close Approaches To The Earth, Minor Planet Center
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• (154276) 2002 SY50 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (154276) 2002 SY50 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary
• (154276) 2002 SY50 at the JPL Small-Body Database
Minor planets navigator
• (154276) 2002 SY50
Small Solar System bodies
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(15430) 1998 UR31
(15430) 1998 UR31 is a main-belt binary asteroid. It was discovered through the Beijing Schmidt CCD Asteroid Program at the Xinglong Station in the Chinese province of Hebei on October 22, 1998. [1] A moon was discovered orbiting the asteroid in 2010. The moon has an orbital period of almost exactly a day, and is tidally locked with the asteroid. [2]
(15430) 1998 UR31
Discovery[1]
Discovered bySCAP
Discovery siteBeijing Xinglong Obs.
Discovery date22 October 1998
Designations
MPC designation
(15430) 1998 UR31
Alternative designations
1998 UR31; 1980 EK1
2000 AB153
Minor planet category
main-belt
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc22044 days (60.35 yr)
Aphelion2.6001 AU (388.97 Gm)
Perihelion1.8433 AU (275.75 Gm)
Semi-major axis
2.2217 AU (332.36 Gm)
Eccentricity0.17032
Orbital period (sidereal)
3.31 yr (1209.6 d)
Mean anomaly
245.22°
Mean motion
0° 17m 51.468s / day
Inclination8.1801°
Longitude of ascending node
62.806°
Argument of perihelion
177.42°
Earth MOID0.829914 AU (124.1534 Gm)
Physical characteristics
Synodic rotation period
2.52735 h (0.105306 d)
Absolute magnitude (H)
14.2
See also
• List of minor planets: 15001–16000
References
1. "JPL Small-Body Database Browser: 15430 (1998 UR31)" (2015-01-28 last obs.). Jet Propulsion Laboratory. Retrieved 5 April 2016.
2. Johnston, Robert. "(15430) 1998 UR31". johnstonsarchive.net. Retrieved 29 May 2015.
External links
• Asteroids with Satellites, Robert Johnston, johnstonsarchive.net
• (15430) 1998 UR31 at the JPL Small-Body Database
Minor planets navigator
• (15430) 1998 UR31
• (15431) 1998 UQ32
Small Solar System bodies
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Asteroid
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Authority control databases
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• MPC | 17 | 0 |
(15502) 1999 NV27
(15502) 1999 NV27 (provisional designation 1999 NV27) is a Jupiter trojan from the Trojan camp, approximately 53 kilometers (33 miles) in diameter. It was discovered on 14 July 1999, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. [1] The dark Jovian asteroid has a rotation period of 15.1 hours and belongs to the 90 largest Jupiter trojans. [8] It has not been named since its numbering in June 2000. [10]
(15502) 1999 NV27
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date14 July 1999
Designations
MPC designation
(15502) 1999 NV27
Alternative designations
1999 NV27 · 1982 BX14
1990 UP2
Minor planet category
Jupiter trojan[1][2]
Trojan[3] · background[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc36.31 yr (13,263 d)
Aphelion5.2093 AU
Perihelion5.0403 AU
Semi-major axis
5.1248 AU
Eccentricity0.0165
Orbital period (sidereal)
11.60 yr (4,238 d)
Mean anomaly
26.357°
Mean motion
0° 5m 6s / day
Inclination16.824°
Longitude of ascending node
308.72°
Argument of perihelion
181.57°
Jupiter MOID0.1096 AU
TJupiter2.9150
Physical characteristics
Mean diameter
50.86±2.51 km[5]
53.10±0.12 km[6]
Synodic rotation period
15.129±0.002 h[7][lower-alpha 1]
Geometric albedo
0.067±0.007[5]
0.069±0.021[6]
Spectral type
C (assumed)[8]
B–V = 0.766±0.047[9]
V–R = 0.445±0.036[9]
V–I = 0.875±0.048[9]
Absolute magnitude (H)
9.9[6]
10.0[1][2][8]
10.10[5]
Orbit and classification
1999 NV27 is a dark Jovian asteroid in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's L5 Lagrangian point, 60° behind its orbit (see Trojans in astronomy). [3] It is also a non-family asteroid of the Jovian background population. [4]
It orbits the Sun at a distance of 5.0–5.2 AU once every 11 years and 7 months (4,238 days; semi-major axis of 5.12 AU). Its orbit has an eccentricity of 0.02 and an inclination of 17° with respect to the ecliptic. [2] The body's observation arc begins with its first observation as 1982 BX14 at Palomar Observatory in January 1982, more than 16 years prior to its official discovery observation at Socorro. [1]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 21 June 2000 (M.P.C. 40827). [10] As of 2021, it has not been named. [1]
Physical characteristics
1999 NV27 is an assumed, carbonaceous C-type asteroid. [8] It has a V–I color index of 0.875. [9]
Rotation period
In September 2009, a first rotational lightcurve of 1999 NV27 was obtained from photometric observations by Linda French at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of 15.03±0.03 hours with a brightness variation of 0.10 magnitude (U=2). [8][11]
Since then, follow-up observations by Daniel Coley and Robert Stephens at the Center for Solar System Studies during 2013–2017 gave four more refined lightcurves, with the best-rated one from January 2017 showing a rotation period of 15.129±0.002 hours and an amplitude of 0.26 magnitude (U=3). [7][12][13][14][lower-alpha 1]
Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1999 NV27 measures 50.86 and 53.10 kilometers in diameter and its surface has an albedo of 0.067 and 0.069, respectively. [5][6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 55.67 kilometers based on an absolute magnitude of 10.0. [8]
100+ largest Jupiter trojans
Largest Jupiter Trojans by survey(A)
(mean-diameter in kilometers; YoD: Year of Discovery)
Designation H WISE IRAS Akari Ln RP V–I YoD Ref
624 Hektor7.2225233230.99L46.920.9301907list
617 Patroclus8.19140.362140.92140.85L5102.800.8301906list
911 Agamemnon7.89131.038166.66185.30L46.590.9801919list
588 Achilles8.67130.099135.47133.22L47.310.9401906list
3451 Mentor8.4126.288116.30117.91L57.700.7701984list
3317 Paris8.3118.790116.26120.45L57.090.9501984list
1867 Deiphobus8.3118.220122.67131.31L558.660.9301971list
1172 Äneas8.33118.020142.82148.66L58.710.9501930list
1437 Diomedes8.3117.786164.31172.60L424.490.8101937list
1143 Odysseus7.93114.624125.64130.81L410.110.8601930list
2241 Alcathous8.64113.682114.63118.87L57.690.9401979list
659 Nestor8.99112.320108.87107.06L415.980.7901908list
3793 Leonteus8.7112.04686.2687.58L45.620.7801985list
3063 Makhaon8.4111.655116.14114.34L48.640.8301983list
1583 Antilochus8.6108.842101.62111.69L431.540.9501950list
884 Priamus8.81101.09396.29119.99L56.860.9001917list
1208 Troilus8.99100.477103.34111.36L556.170.7401931list
1173 Anchises8.8999.549126.27120.49L511.600.7801930list
2207 Antenor8.8997.65885.1191.32L57.970.9501977list
2363 Cebriones9.1195.97681.8484.61L520.050.9101977list
4063 Euforbo8.795.619102.46106.38L48.850.9501989list
2357 Phereclos8.9494.62594.9098.45L514.390.9601981list
4709 Ennomos8.591.43380.8580.03L512.280.6901988list
2797 Teucer8.789.430111.14113.99L410.150.9201981list
2920 Automedon8.888.574111.01113.11L410.210.9501981list
15436 Dexius9.187.64685.7178.63L48.970.8701998list
3596 Meriones9.287.38075.0973.28L412.960.8301985list | 18 | 0 |
2893 Peiroos9.2386.88487.4686.76L58.960.9501975list
4086 Podalirius9.185.49586.8985.98L410.430.8701985list
4060 Deipylos9.384.04379.2186.79L49.300.7601987list
1404 Ajax9.383.99081.6996.34L429.380.9601936list
4348 Poulydamas9.582.03270.0887.51L59.910.8401988list
5144 Achates9.080.95891.9189.85L55.960.9201991list
4833 Meges8.980.16587.3389.39L414.250.9401989list
2223 Sarpedon9.4177.48094.63108.21L522.740.8801977list
4489 Dracius9.076.59592.9395.02L412.580.9501988list
2260 Neoptolemus9.3176.43571.6581.28L48.180.9501975list
5254 Ulysses9.276.14778.3480.00L428.720.9701986list
3708 Socus9.375.66179.5976.75L56.550.9801974list
2674 Pandarus9.174.26798.10101.72L58.481.0001982list
3564 Talthybius9.473.73068.9274.11L440.590.9001985list
4834 Thoas9.172.33186.8296.21L418.190.9501989list
7641 Cteatus9.471.83968.9775.28L427.770.9801986list
3540 Protesilaos9.370.22576.8487.66L48.950.9401973list
11395 Iphinous9.868.97764.7167.78L417.38–1998list
4035 Thestor9.668.73368.2366.99L413.470.9701986list
5264 Telephus9.468.47273.2681.38L49.530.9701991list
1868 Thersites9.568.16370.0878.89L410.480.9601960list
9799 Thronium9.668.03364.8772.42L421.520.9101996list
4068 Menestheus9.567.62562.3768.46L414.400.9501973list
23135 Pheidas9.966.23058.2968.50L48.690.8602000list
2456 Palamedes9.365.91691.6699.60L47.240.9201966list
3709 Polypoites9.165.29799.0985.23L410.041.0001985list
1749 Telamon9.564.89881.0669.14L416.980.9701949list
3548 Eurybates9.663.88572.1468.40L48.710.7301973list
4543 Phoinix9.763.83662.7969.54L438.871.2001989list
12444 Prothoon9.863.83564.3162.41L515.82–1996list
4836 Medon9.563.27767.7378.70L49.820.9201989list
16070 Charops9.763.19164.1368.98L520.240.9601999list
15440 Eioneus9.662.51966.4871.88L421.430.9701998list
4715 Medesicaste9.762.09763.9165.93L58.810.8501989list
34746 Thoon9.861.68460.5163.63L519.630.9502001list
38050 Bias9.861.60361.0450.44L418.850.9901998list
5130 Ilioneus9.760.71159.4052.49L514.770.9601989list
5027 Androgeos9.659.78657.86n.a.L411.380.9101988list
6090 Aulis9.459.56874.5381.92L418.480.9801989list
5648 Axius9.759.29563.91n.a.L537.560.9001990list
7119 Hiera9.759.15076.4077.29L44000.9501989list
4805 Asteropaios10.057.64753.1643.44L512.37–1990list
16974 Iphthime9.857.34155.4357.15L478.90.9601998list
4867 Polites9.857.25158.2964.29L511.241.0101989list
2895 Memnon10.056.70655.67n.a.L57.500.7101981list
4708 Polydoros9.954.96455.67n.a.L57.520.9601988list
(21601) 1998 XO8910.054.90955.6756.08L412.650.9701998list
12929 Periboea9.954.07761.0455.34L59.270.8801999list
17492 Hippasos10.053.97555.67n.a.L517.75–1991list
5652 Amphimachus10.153.92153.1652.48L48.371.0501992list
2759 Idomeneus9.953.67661.0152.55L432.380.9101980list
5258 Rhoeo10.253.27550.77n.a.L419.851.0101989list
(12126) 1999 RM1110.153.202n.a.n.a.L5n.a. ?1999list
(15502) 1999 NV2710.053.10055.6750.86L515.130.8751999list
4754 Panthoos10.053.02553.1556.96L527.68–1977list
4832 Palinurus10.052.05853.16n.a.L55.321.0001988list
5126 Achaemenides10.551.92244.2248.57L453.02–1989list
3240 Laocoon10.251.69550.77n.a.L511.310.8801978list
4902 Thessandrus9.851.26361.0471.79L47380.9601989list
11552 Boucolion10.151.13653.1653.91L532.44–1993list
(20729) 1999 XS14310.450.96146.30n.a.L45.721.0001999list
6545 Leitus10.150.95153.16n.a.L416.260.9101986list
4792 Lykaon10.150.87053.16n.a.L540.090.9601988list
21900 Orus10.050.81055.6753.87L413.450.9501999list
1873 Agenor10.150.79953.7654.38L520.60–1971list
5028 Halaesus10.250.77050.77n.a.L424.940.9001988list
2146 Stentor9.950.75558.29n.a.L416.40–1976list
4722 Agelaos10.050.37853.1659.47L518.440.9101977list
5284 Orsilocus10.150.15953.16n.a.L410.310.9701989list
11509 Thersilochos10.149.96053.1656.23L517.37–1990list
5285 Krethon10.149.60658.5352.61L412.041.0901989list
4791 Iphidamas10.149.52857.8559.96L59.701.0301988list
9023 Mnesthus10.149.15150.7760.80L530.66–1988list | 18 | 1 |
5283 Pyrrhus9.748.35664.5869.93L47.320.9501989list
4946 Askalaphus10.248.20952.7166.10L422.730.9401988list
(22149) 2000 WD4910.248.19050.7750.37L47.841.0902000list
(32496) 2000 WX18210.248.01750.7751.63L523.340.9502000list
5120 Bitias10.247.98750.77n.a.L515.210.7801988list
12714 Alkimos10.147.81961.0454.62L428.48–1991list
7352 Hypsenor9.947.73155.67 47.07L56480.8501994list
1870 Glaukos10.647.64942.23n.a.L55.99—1971list
4138 Kalchas10.146.46253.1661.04L429.20.8101973list
(23958) 1998 VD3010.246.00150.7747.91L45620.9901998list
4828 Misenus10.445.95446.30 43.22L512.870.9201988list
4057 Demophon10.145.68353.16n.a.L429.821.0601985list
4501 Eurypylos10.445.52446.30n.a.L46.05–1989list
4007 Euryalos10.345.51548.4853.89L46.39–1973list
5259 Epeigeus10.344.74142.5944.42L418.42–1989list
30705 Idaios10.444.54646.30n.a.L515.74–1977list
16560 Daitor10.743.86151.4243.38L5––1991list
(15977) 1998 MA1110.443.53046.3051.53L52500.9061998list
7543 Prylis10.642.89342.23n.a.L417.80–1973list
4827 Dares10.542.77044.22n.a.L519.00–1988list
1647 Menelaus10.542.71644.22n.a.L417.740.8661957list
(A) Used sources: WISE/NEOWISE catalog (NEOWISE_DIAM_V1 PDS, Grav, 2012); IRAS data (SIMPS v.6 catalog); and Akari catalog (Usui, 2011); RP: rotation period and V–I (color index) taken from the LCDB
Note: missing data was completed with figures from the JPL SBDB (query) and from the LCDB (query form) for the WISE/NEOWISE and SIMPS catalogs, respectively. These figures are given in italics. Also, listing is incomplete above #100.
Notes
1. Lightcurve plots of (15502) 1999 NV27 from Aug 2013, Oct 2014, Dec 2015 and Jan 2017 by Daniel Coley and Robert Stephens at the Center for Solar System Studies (U80) and (U81). Quality code is 3/2+/3/3 (lightcurve rating at CS3). Summary figures at the LCDB and CS3.
References
1. "15502 (1999 NV27)". Minor Planet Center. Retrieved 20 June 2018.
2. "JPL Small-Body Database Browser: 15502 (1999 NV27)" (2018-05-24 last obs.). Jet Propulsion Laboratory. Retrieved 20 June 2018.
3. "List of Jupiter Trojans". Minor Planet Center. 1 June 2018. Retrieved 20 June 2018.
4. "Asteroid (15502) 1999 NV27 – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 20 June 2018.
5. Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
6. Grav, T.; Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.; Nugent, C. R. (November 2012). "WISE/NEOWISE Observations of the Jovian Trojan Population: Taxonomy". The Astrophysical Journal. 759 (1): 10. arXiv:1209.1549. Bibcode:2012ApJ...759...49G. doi:10.1088/0004-637X/759/1/49. S2CID 119101711. (online catalog)
7. Stephens, Robert D.; Coley, Daniel R. (July 2017). "Lightcurve Analysis of Trojan Asteroids at the Center for Solar System Studies 2017 January - March". The Minor Planet Bulletin. 44 (3): 252–257. Bibcode:2017MPBu...44..252S. ISSN 1052-8091. PMC 7243922. PMID 32455404.
8. "LCDB Data for (15502)". Asteroid Lightcurve Database (LCDB). Retrieved 20 June 2018.
9. Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited". Astronomy and Astrophysics. 546: 20. arXiv:1209.1896. Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. S2CID 54776793.
10. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 June 2018.
11. French, Linda M.; Stephens, Robert D.; Coley, Daniel R.; Wasserman, Lawrence H.; Vilas, Faith; La Rocca, Daniel (October 2013). "A Troop of Trojans: Photometry of 24 Jovian Trojan Asteroids". The Minor Planet Bulletin. 40 (4): 198–203. Bibcode:2013MPBu...40..198F. ISSN 1052-8091.
12. Stephens, Robert D.; Coley, Daniel R.; Warner, Brian D.; French, Linda M. (October 2016). "Lightcurves of Jovian Trojan Asteroids from the Center for Solar System Studies: L4 Greek Camp and Spies". The Minor Planet Bulletin. 43 (4): 323–331. Bibcode:2016MPBu...43..323S. ISSN 1052-8091.
13. Stephens, Robert D.; French, Linda M.; Davitt, Chelsea; Coley, Daniel R. (April 2014). "At the Scaean Gates: Observations Jovian Trojan Asteroids, July- December 2013". The Minor Planet Bulletin. 41 (2): 95–100. Bibcode:2014MPBu...41...95S. ISSN 1052-8091.
14. Stephens, Robert D.; Coley, Daniel R.; French, Linda M. (July 2015). "Dispatches from the Trojan Camp - Jovian Trojan L5 Asteroids Observed from CS3: 2014 October - 2015 January". The Minor Planet Bulletin. 42 (3): 216–224. Bibcode:2015MPBu...42R.216S. ISSN 1052-8091.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• Asteroid (15502) 1999 NV27 at the Small Bodies Data Ferret
• (15502) 1999 NV27 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (15502) 1999 NV27 at the JPL Small-Body Database | 18 | 2 |
Minor planets navigator
• 15501 Pepawlowski
• (15502) 1999 NV27
Small Solar System bodies
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• Meanings of names
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(15692) 1984 RA
(15692) 1984 RA (provisional designation 1984 RA) is a Hungaria asteroid from the innermost regions of the asteroid belt, approximately 2 kilometers (1.2 miles) in diameter. It was discovered on 1 September 1984, by Italian astronomer Maria Barucci at the Palomar Observatory in California, United States. [1] The presumed E-type asteroid has a longer-than average rotation period of 37.4 hours and possibly an elongated shape. [3]
(15692) 1984 RA
Discovery[1]
Discovered byM. Barucci
Discovery sitePalomar Obs.
Discovery date1 September 1984
Designations
MPC designation
(15692) 1984 RA
Alternative designations
1984 RA · 1986 JT1
1992 SZ26
Minor planet category
main-belt · (inner)[2]
Hungaria[1][3][4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc41.44 yr (15,135 d)
Aphelion2.1225 AU
Perihelion1.7302 AU
Semi-major axis
1.9264 AU
Eccentricity0.1018
Orbital period (sidereal)
2.67 yr (977 d)
Mean anomaly
138.59°
Mean motion
0° 22m 6.96s / day
Inclination23.217°
Longitude of ascending node
142.60°
Argument of perihelion
273.05°
Physical characteristics
Mean diameter
1.728±0.273 km[5][6]
2.43 km (calculated)[3]
Synodic rotation period
37.44±0.05 h[7][lower-alpha 1]
Geometric albedo
0.30 (assumed)[3]
0.780±0.146[5][6]
Spectral type
E (assumed)[3]
Absolute magnitude (H)
14.7[6]
14.85±0.97[8]
14.9[2]
15.0[3]
Orbit and classification
1984 RA is a bright core member of the Hungaria family (003),[4] a large family of three thousand asteroids located within the dynamical group with the same name. [1][3] Hungarias form the innermost dense concentration of asteroids in the Solar System; they are inside the asteroid belt's core region, sometimes considered a completely independent population. [9]
The asteroid orbits the Sun in the innermost asteroid belt at a distance of 1.7–2.1 AU once every 2 years and 8 months (977 days; semi-major axis of 1.93 AU). Its orbit has an eccentricity of 0.10 and an inclination of 23° with respect to the ecliptic. [2] The body's observation arc begins with a precovery found in the Digitized Sky Survey and taken at the Siding Spring Observatory in November 1977, almost 7 years prior to its official discovery observation at Palomar. [1]
Physical characteristics
1984 RA is an assumed E-type asteroid, known for their high albedos, typically around 0.4. [3]
Rotation period
In July 2013, a rotational lightcurve of this asteroid was obtained from photometric observations by American astronomer Brian Warner at the Palmer Divide Station (U82) in California. Lightcurve analysis gave a long rotation period of 37.44 hours with a brightness amplitude of 0.66 magnitude, indicative of an elongated shape (U=2). [7][lower-alpha 1] While not being a slow rotator, 1984 RA has a significantly longer period than most asteroids, which rotate once every 2 to 20 hours around their axis.
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, this asteroid measures 1.728 kilometers in diameter and its surface has an exceptionally high albedo of 0.78. [5][6] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.30 – a compromise value between the E- (0.40) and S-type (0.20) members of the Hungaria family and group, respectively – and calculates a diameter of 2.43 kilometers based on an absolute magnitude of 15.0. [3]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). [10] As of 2018, it has not been named. [1]
Notes
1. Lightcure plot of (15692) 1984 RA, by B. D. Warner at the Center for Solar System Studies – Palmer Divide Station (U82). Rotation period 37.44±0.05 hours. Observation from 8 Jul 2013 to 1 Aug 2013. Data points: 273. Quality code is 2. Summary figures at the LCDB
References
1. "15692 (1984 RA)". Minor Planet Center. Retrieved 10 May 2018.
2. "JPL Small-Body Database Browser: 15692 (1984 RA)" (2018-04-26 last obs.). Jet Propulsion Laboratory. Retrieved 10 May 2018.
3. "LCDB Data for (15692)". Asteroid Lightcurve Database (LCDB). Retrieved 10 May 2018.
4. "Asteroid (15692) 1984 RA – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. S2CID 118745497.
6. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID 118700974. (catalog)
7. Warner, Brian D. (January 2014). "Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2013 June- September". The Minor Planet Bulletin. 41 (1): 27–32. Bibcode:2014MPBu...41...27W. ISSN 1052-8091.
8. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339.
9. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. S2CID 119280014.
10. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 10 May 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• (15692) 1984 RA at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info | 19 | 0 |
• (15692) 1984 RA at the JPL Small-Body Database
Minor planets navigator
• 15691 Maslov
• (15692) 1984 RA
Small Solar System bodies
Minor planets
• Designation
• Groups
• List
• Moon
• Meanings of names
Asteroid
• Active
• Aten asteroid
• Asteroid belt
• Family
• Jupiter trojan
• Near-Earth
• Spectral types
Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
• Extinct
• Great
• Halley-type
• Hyperbolic
• Long-period
• Lost
• Near-parabolic
• Periodic
• Sungrazing
Other
• Cosmic dust
• Meteoroids
• Space debris
Authority control databases
• JPL SBDB
• MPC | 19 | 1 |
(15700) 1987 QD
(15700) 1987 QD (provisional designation 1987 QD) is a Mars-crossing asteroid and a binary candidate from inside the innermost region of the asteroid belt, approximately 3 kilometers (1.9 miles) in diameter. It was discovered on 24 August 1987, by American astronomer Stephen Singer-Brewster at the Palomar Observatory in California. [1] The likely spherical X-type asteroid has a rotation period of 3.1 hours. The suspected presence of a kilometer-sized minor-planet moon was announced in November 2000. [3]
(15700) 1987 QD
Discovery[1]
Discovered byS. Singer-Brewster
Discovery sitePalomar Obs.
Discovery date24 August 1987
Designations
MPC designation
(15700) 1987 QD
Alternative designations
1987 QD · 2000 JD1
Minor planet category
Mars-crosser[1][2]
binary[3][4][5]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc63.65 yr (23,249 d)
Aphelion2.9047 AU
Perihelion1.5136 AU
Semi-major axis
2.2092 AU
Eccentricity0.3148
Orbital period (sidereal)
3.28 yr (1,199 d)
Mean anomaly
132.51°
Mean motion
0° 18m 0.72s / day
Inclination26.788°
Longitude of ascending node
175.47°
Argument of perihelion
119.47°
Known satellites1 (strong candidate)[3][6]
Earth MOID0.6219 AU (242 LD)
Physical characteristics
Mean diameter
2.95±0.29 km[7]
3.04 km (derived)[4]
Synodic rotation period
3.0586±0.0001 h[6][lower-alpha 1]
Geometric albedo
0.20 (assumed)[4]
0.268±0.054[7]
Spectral type
X (Pan-STARRS)[4][8]
X (SDSS-MOC)[9]
S[4][10]
Absolute magnitude (H)
14.50±0.07 (R)[lower-alpha 1]
14.70[1][2][7]
14.99±0.086[4][11]
Orbit and classification
1987 QD is a Mars-crossing asteroid, a member of the dynamically unstable group, located between the main belt and near-Earth populations, and crossing the orbit of Mars at 1.666 AU. It orbits the Sun inside the innermost region of the asteroid belt at a distance 1.5–2.9 AU once every 3 years and 3 months (1,199 days; semi-major axis of 2.21 AU). Its orbit has an eccentricity of 0.31 and an inclination of 27° with respect to the ecliptic. [2]
The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar in May 1954, more than 33 years prior to its official discovery observation. [1] It will pass 6,352,000 km (0.04246 AU) from the main-belt asteroid 7 Iris on 3 September 2173. [2]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40991). [12] As of 2018, it has not been named. [1]
Physical characteristics
In the SDSS-based taxonomy and according to the survey conducted by Pan-STARRS, 1987 QD is an X-type asteroid. [4][8][9] It has also been classified as a common, stony S-type asteroid. [4][10]
Rotation period
In September 2010, a first rotational lightcurve of 1987 QD was obtained from photometric observations by Brian Skiff. Lightcurve analysis gave a rotation period of 3.068 hours and a brightness variation of 0.07 magnitude (U=3-). [4][lower-alpha 2] Within less than two weeks, follow-up observations by a large international collaboration of astronomers determined a refined period of 3.0586±0.0001 hours with a low amplitude of 0.07 magnitude, indicating that the body has a spherical shape (U=3). [6][lower-alpha 1] An alternative observation that gave a tentative period 9.709 hours received a poor quality rating (U=1). [4][13]
Strong binary candidate
The photometric observations during September and October 2010 revealed that 1987 QD is a candidate for a synchronous binary asteroid with a minor-planet moon orbiting it every 50.3±0.5 hours at an estimated average distance of 14 km. [3] The findings were announced on 6 November 2009. [6] The lightcurve indicated mutual occultation events, however, a conclusive solution for the orbit period was not obtained. [lower-alpha 3] The Johnston's archive estimates a diameter of 1.23 kilometer for the satellite, or 31% the size of its primary. [3]
The international collaboration included Richard Durkee at the Shed of Science Observatory (H39), Petr Pravec, Kamil Hornoch and Peter Kušnirák at Ondřejov Observatory, Donald Pray at Carbuncle Hill Observatory (912), David Higgins at Canberra (E14), Jozef Világi and Štefan Gajdoš at Modra Observatory, Judit Györgyey Ries at McDonald Observatory and Julian Oey at Leura Observatory (E17), as well as astronomers at the Kharkiv Kharkov (101), Simeiz and Skalnate Pleso observatories. [6]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 1987 QD measures 2.95 kilometers in diameter and its surface has an albedo of 0.268,[7] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and derives a diameter of 3.04 kilometers based on an absolute magnitude of 14.99. [4]
Notes
1. Lightcurve plot of (15700) 1987 QD from Ondrejov data obtained by the NEO Photometric Program and collaborating projects. Period 3.0586±0.0001 hours with a brightness amplitude of 0.07±0.01 mag. Quality code is 3. Summary figures at the LCDB and Pravec, P.; Wolf, M.; Sarounova, L. (2010) (data sheet).
2. Skiff (2011) web: rotation period 3.068±0.003 hours with a brightness amplitude of mag. Quality code is 3-. Summary figures at the LCDB
3. There are two possible orbital periods for the secondary: 50.3 and 62.9 hours. Neither could be conclusively established. LCDB
References
1. "15700 (1987 QD)". Minor Planet Center. Retrieved 5 July 2018.
2. "JPL Small-Body Database Browser: 15700 (1987 QD)" (2018-01-20 last obs.). Jet Propulsion Laboratory. Retrieved 5 July 2018.
3. Johnston, Wm. Robert (19 February 2017). "Asteroids with Satellites Database – (15700) 1987 QD". Johnston's Archive. Retrieved 5 July 2018. (at Data Ferret)
4. "LCDB Data for (15700)". Asteroid Lightcurve Database (LCDB). Retrieved 5 July 2018.
5. "Asteroid (15700) 1987 QD". Small Bodies Data Ferret. Retrieved 5 July 2018.
6. Durkee, R.; Pravec, P.; Hornoch, K.; Kusnirak, P.; Pray, D.; Brookfield, W.; et al. (November 2010). "(15700) 1987 QD". Central Bureau Electronic Telegrams. 2540 (2540): 1. Bibcode:2010CBET.2540....1D. Retrieved 5 July 2018.
7. Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data". Astronomy and Astrophysics. 603: 8. arXiv:1705.10263. Bibcode:2017A&A...603A..55A. | 20 | 0 |
doi:10.1051/0004-6361/201629917. S2CID 119224590.
8. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339.
9. Carvano, J. M.; Hasselmann, P. H.; Lazzaro, D.; Mothé-Diniz, T. (February 2010). "SDSS-based taxonomic classification and orbital distribution of main belt asteroids". Astronomy and Astrophysics. 510: 12. Bibcode:2010A&A...510A..43C. doi:10.1051/0004-6361/200913322. Retrieved 30 October 2019. (PDS data set)
10. Carry, B.; Solano, E.; Eggl, S.; DeMeo, F. E. (April 2016). "Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry". Icarus. 268: 340–354. arXiv:1601.02087. Bibcode:2016Icar..268..340C. doi:10.1016/j.icarus.2015.12.047. S2CID 119258489.
11. Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026.
12. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 5 July 2018.
13. Vander Haagen, Gary A. (April 2011). "Lightcurves of 10452 ZUEV, (14657) 1998 YU27, and (15700) 1987 QD". The Minor Planet Bulletin. 38 (2): 71–72. Bibcode:2011MPBu...38...71V. ISSN 1052-8091.
External links
• CBET 2540 – (15700) 1987 QD Central Bureau for Astronomical Telegrams, 6 Nov 2010
• Asteroids with Satellites, Robert Johnston, johnstonsarchive.net
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• (15700) 1987 QD at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (15700) 1987 QD at the JPL Small-Body Database
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• 15699 Lyytinen
• (15700) 1987 QD
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15810 Arawn
15810 Arawn (provisional designation 1994 JR1) is a trans-Neptunian object (TNO) from the inner regions of the Kuiper belt, approximately 133 kilometres (83 mi) in diameter. It belongs to the plutinos, the most populous class of resonant TNOs. It was named after Arawn, the ruler of the underworld in Welsh mythology, and was discovered on 12 May 1994, by astronomers Michael Irwin and Anna Żytkow with the 2.5-metre Isaac Newton Telescope at Roque de los Muchachos Observatory in the Canary Islands, Spain. [1]
15810 Arawn
A distant view of Arawn (center) from New Horizons in November 2015. [n 1]
Discovery[1]
Discovered byM. J. Irwin
A. Żytkow
Discovery siteLa Palma Obs.
Discovery date12 May 1994
Designations
MPC designation
(15810) Arawn
Pronunciation/ˈɑːraʊn/[2]
Named after
Arawn (Welsh mythology)[1]
Alternative designations
1994 JR1
Minor planet category
TNO · plutino[3][4]
Orbital characteristics[5]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 2
Observation arc21.91 yr (8,002 days)
Aphelion44.241 AU
Perihelion34.720 AU
Semi-major axis
39.480 AU
Eccentricity0.1206
Orbital period (sidereal)
248.07 yr (90,609 days)
Mean anomaly
30.638°
Mean motion
0° 0m 14.4s / day
Inclination3.8074°
Longitude of ascending node
144.69°
Argument of perihelion
101.89°
Physical characteristics
Dimensions133 km (83 mi)[6]
145 km (90 mi)[7]
Synodic rotation period
5.47±0.33 h[8]
Geometric albedo
0.04[8]
Absolute magnitude (H)
7.6[5]
Arawn is unusual in that it has been observed at a much closer distance than most Kuiper belt objects, by the New Horizons spacecraft, which imaged it from a distance of 111 million km (69 million mi; 0.74 AU) in April 2016; this and its other observations have allowed its rotation period to be determined. [7][9]
Orbit and physical properties
Arawn is moving in a relatively eccentric orbit entirely beyond the orbit of Neptune. With a semi-major axis of 39.4 AU, it orbits the Sun once every 247 years and 6 months (90,409 days). Its orbit has a perihelion (closest approach to the Sun) of 34.7 AU, an aphelion (farthest distance from the Sun) of 44.1 AU, an eccentricity of 0.12, and an inclination of 4° with respect to the ecliptic. [5] It is a plutino, being trapped in a 2:3 mean motion resonance with Neptune, similarly to dwarf planet Pluto, the largest known plutino.
It measures approximately 133 km (83 mi) in diameter,[6] based on an absolute magnitude of 7.6, and an estimated albedo of 0.1. Observations by the Hubble Space Telescope show that Arawn has a very red surface. [10] In April 2016, its rotation period of 5.47 hours was determined. [9]
Quasi-satellite dynamical state and orbital evolution
In 2012 Arawn was hypothesized to be in a quasi-satellite loop around Pluto, as part of a recurring pattern, becoming a Plutonian quasi-satellite every 2 Myr and remaining in that phase for nearly 350,000 years. [11][12] Measurements made by the New Horizons probe in 2015 made it possible to calculate the motion of Arawn much more accurately. [8] These calculations confirm the general dynamics described in the hypotheses. [13] However, it is not agreed upon among astronomers whether Arawn should be classified as a quasi-satellite of Pluto based on this motion since its orbit is primarily controlled by Neptune with only occasional smaller perturbations caused by Pluto. [8][9][13]
Origin
Arawn is moving in a very stable orbit, likely as stable as Pluto's. This suggests that it might be a primordial plutino formed around the same time Pluto itself and Charon came into existence. It is unlikely to be relatively recent debris that originated in collisions within Pluto's system or a captured object. [11]
Observation
Arawn is currently relatively close to Pluto. In 2017 it was only 2.7 AU from Pluto. [14] Before 486958 Arrokoth was discovered in 2014, Arawn was the best known target for a flyby by the New Horizons spacecraft after its Pluto flyby in 2015. [15][16]
Arawn was one of the first objects targeted for distant observations by New Horizons, which were taken on 2 November 2015. [17] More observations were made in April 2016. [7]
On 2 November 2015, Arawn was imaged by the LORRI instrument aboard New Horizons, making it the closest observation of a Kuiper belt object other than the Pluto–Charon system by a factor of 15. [18]
Between 7–8 April 2016, New Horizons imaged Arawn from a new record distance of about 111 million kilometres, using the LORRI instrument. The new images allowed the science team at Southwest Research Institute (SwRI) in Boulder, Colorado, to further pinpoint the location of Arawn to within 1000 kilometers. The new data also made it possible for scientists to observe its rotation period, which was determined to be 5.47 hours. [9]
On 15 April 2024, the James Webb Space Telescope (JWST) conducted an observation of the Kuiper Belt object Arawn for a duration of 1 minute and 4 seconds using its NIRCam instrument in Moving Target mode with published findings expected at a later date. [19]
• April 2016 observations of Arawn by New Horizons
• Trajectory of New Horizons and other nearby Kuiper belt objects
• Orbit of Arawn near Pluto
Arawn occulted a star on 25 August 2022. [20]
See also
• Kuiper belt
• List of trans-Neptunian objects
References
1. "(15810) Arawn". IAU Minor Planet Center. Archived from the original on 27 October 2017. Retrieved 17 January 2017.
2. Matthieu Boyd, trans., The Four Branches of The Mabinogi, Broadview Press, 2017
3. Marc W. Buie (14 October 2006). "Orbit Fit and Astrometric record for 15810". SwRI (Space Science Department). Archived from the original on 14 February 2012. Retrieved 2 October 2008.
4. Brian G. Marsden (17 July 2008). "MPEC 2008-O05 : Distant Minor Planets (2008 Aug. 2.0 TT)". IAU Minor Planet Center. Archived from the original on 3 May 2020. Retrieved 26 August 2016.
5. "JPL Small-Body Database Browser: 15810 (1994 JR1)" (2016-04-08 last obs.). Jet Propulsion Laboratory. Archived from the original on 10 March 2020. Retrieved 26 August 2016.
6. "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 13 March 2002. Retrieved 26 August 2016.
7. "Catalog Page for PIA20589". Archived from the original on 5 November 2016. Retrieved 5 November 2016.
8. Porter, Simon B.; et al. (2016). "The First High-phase Observations of a KBO: New Horizons Imaging of (15810) 1994 JR1 from the Kuiper Belt". The Astrophysical Journal Letters. 828 (2): L15. arXiv:1605.05376. Bibcode:2016ApJ...828L..15P. doi:10.3847/2041-8205/828/2/L15. S2CID 54507506.
9. "New Horizons Collects First Science on a Post-Pluto Object". New Horizons. NASA/JHUAPL/SwRI. 17 May 2016. Archived from the original on 7 June 2016. Retrieved 26 August 2016.
10. | 21 | 0 |
"Scientists Determine Color of Kuiper Belt Objects JR1 and MU69 | Planetary Science, Space Exploration". Sci-News.com. Archived from the original on 4 November 2016. Retrieved 2 November 2016.
11. de la Fuente Marcos, C.; de la Fuente Marcos, R. (November 2012). "Plutino 15810 (1994 JR1), an accidental quasi-satellite of Pluto". Monthly Notices of the Royal Astronomical Society: Letters. 427 (1): L85–L89. arXiv:1209.3116. Bibcode:2012MNRAS.427L..85D. doi:10.1111/j.1745-3933.2012.01350.x. S2CID 118570875.
12. "Pluto's fake moon". Sky & Telescope. 24 September 2012. Archived from the original on 1 July 2015. Retrieved 24 September 2012.
13. de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (2016). "The analemma criterion: accidental quasi-satellites are indeed true quasi-satellites". Monthly Notices of the Royal Astronomical Society. 462 (3): 3344–3349. arXiv:1607.06686. Bibcode:2016MNRAS.462.3344D. doi:10.1093/mnras/stw1833.
14. "50000 Quaoar distance (AU) from Pluto". Archived from the original on 25 February 2012. Retrieved 18 December 2007.
15. Ted Stryk / Emily Lakdawalla (24 January 2011). "Ted Stryk: Report from the 2011 New Horizons Science Team Meeting". The Planetary Society Blog. Archived from the original on 1 July 2011. Retrieved 25 January 2011.
16. "25 closer candidates". Archived from the original on 16 April 2014. Retrieved 30 September 2012.
17. "A Distant Close-up: New Horizons' Camera Captures a Wandering Kuiper Belt Object". New Horizons. NASA/JHUAPL. 4 December 2015. Archived from the original on 8 December 2015. Retrieved 5 December 2015.
18. "New Horizons' catches a wandering Kuiper Belt Object not far off". SpaceDaily. 7 December 2015. Archived from the original on 26 November 2021. Retrieved 8 December 2015.
19. "JWST Schedule". James Webb Space Telescope. Retrieved 17 April 2024.
20. RECON: TNO occultation with 15810 Archived 3 November 2022 at the Wayback Machine - Marc W. Buie
Notes
1. This four-frame animation depicting Arawn was taken on 2 November 2015, by New Horizons, when the spacecraft was 270 million km (170 million mi) away. Arawn is the white dot, just left of center, moving from right to left.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• 15810 Arawn at the JPL Small-Body Database
Minor planets navigator
• (15809) 1994 JS
• 15810 Arawn
• 15811 Nüsslein-Volhard
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• Neptune and Triton
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Logistics
• Atlas V (launch vehicle)
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Related
• Hubble Space Telescope
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Category
Authority control databases
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• MPC | 21 | 1 |
(15977) 1998 MA11
(15977) 1998 MA11 (provisional designation 1998 MA11) is a Jupiter trojan from the Trojan camp, approximately 45 kilometers (28 miles) in diameter. It was discovered on 19 June 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Lab's ETS near Socorro, New Mexico, in the United States. [1] The suspected tumbler is also a slow rotator with a period of 250 hours. [8] It has not been named since its numbering in July 2000. [10]
(15977) 1998 MA11
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date19 June 1998
Designations
MPC designation
(15977) 1998 MA11
Alternative designations
1998 MA11 · 1999 NG2
Minor planet category
Jupiter trojan[1][2]
Trojan[3] · background[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc64.37 yr (23,510 d)
Aphelion5.4295 AU
Perihelion4.9353 AU
Semi-major axis
5.1824 AU
Eccentricity0.0477
Orbital period (sidereal)
11.80 yr (4,309 d)
Mean anomaly
72.300°
Mean motion
0° 5m 0.6s / day
Inclination17.344°
Longitude of ascending node
209.57°
Argument of perihelion
229.49°
Jupiter MOID0.0328 AU
TJupiter2.9070
Physical characteristics
Mean diameter
43.53±0.86 km[5]
51.53±3.86 km[6]
Synodic rotation period
250±5 h[7][lower-alpha 1]
Geometric albedo
0.046[6]
0.071±0.008[5]
Spectral type
C (assumed)[8]
B–V = 0.748±0.033[9]
V–R = 0.465±0.025[9]
V–I = 0.906±0.026[9]
Absolute magnitude (H)
10.30[5]
10.40[1][2][6][8]
Orbit and classification
1998 MA11 is a Jupiter trojan in a 1:1 orbital resonance with Jupiter. It is located in the trailering Trojan camp at the Gas Giant's L5 Lagrangian point, 60° behind its orbit (see Trojans in astronomy). [3]
It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 10 months (4,309 days; semi-major axis of 5.18 AU). Its orbit has an eccentricity of 0.05 and an inclination of 17° with respect to the ecliptic. [2] The body's observation arc begins with a precovery published by the Digitized Sky Survey and taken at Palomar Observatory in December 1953, more than 44 years prior to its official discovery observation at Socorro. [1]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 26 July 2000 (M.P.C. 40994). [10] As of 2021, it has not been named. [1]
Physical characteristics
1998 MA11 is an assumed C-type asteroid. [8] It has a typical V–I color index of 0.906 (see table below). [9]
Rotation period
In August 2013, Robert Stephens at the Center for Solar System Studies observed 1998 MA11 over three nights. However no meaningful rotational lightcurve could be determined, as the lightcurve's amplitude never varied more than 0.02 magnitude. A period of 11.17 hours was only derived for demonstration purpose (U=2-). [11] In December 2015, Stephens obtained an improved lightcurve with a rotation period of 250±5 hours and a brightness variation of 0.30 magnitude (U=2-). This time the asteroid was observed on 16 nights over a period of one month. The photometric observations also revealed that this object possibly has a non-principal axis rotation, which is commonly known as tumbling. [7][8][lower-alpha 1]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer and the Japanese Akari satellite, 1998 MA11 measures 43.53 and 51.53 kilometers in diameter and its surface has an albedo of 0.071 and 0.046, respectively. [5][6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a carbonaceous asteroid of 0.057 and calculates a diameter of 46.30 kilometers based on an absolute magnitude of 10.4. [8]
100+ largest Jupiter trojans
Largest Jupiter Trojans by survey(A)
(mean-diameter in kilometers; YoD: Year of Discovery)
Designation H WISE IRAS Akari Ln RP V–I YoD Ref
624 Hektor7.2225233230.99L46.920.9301907list
617 Patroclus8.19140.362140.92140.85L5102.800.8301906list
911 Agamemnon7.89131.038166.66185.30L46.590.9801919list
588 Achilles8.67130.099135.47133.22L47.310.9401906list
3451 Mentor8.4126.288116.30117.91L57.700.7701984list
3317 Paris8.3118.790116.26120.45L57.090.9501984list
1867 Deiphobus8.3118.220122.67131.31L558.660.9301971list
1172 Äneas8.33118.020142.82148.66L58.710.9501930list
1437 Diomedes8.3117.786164.31172.60L424.490.8101937list
1143 Odysseus7.93114.624125.64130.81L410.110.8601930list
2241 Alcathous8.64113.682114.63118.87L57.690.9401979list
659 Nestor8.99112.320108.87107.06L415.980.7901908list
3793 Leonteus8.7112.04686.2687.58L45.620.7801985list
3063 Makhaon8.4111.655116.14114.34L48.640.8301983list
1583 Antilochus8.6108.842101.62111.69L431.540.9501950list
884 Priamus8.81101.09396.29119.99L56.860.9001917list
1208 Troilus8.99100.477103.34111.36L556.170.7401931list
1173 Anchises8.8999.549126.27120.49L511.600.7801930list
2207 Antenor8.8997.65885.1191.32L57.970.9501977list
2363 Cebriones9.1195.97681.8484.61L520.050.9101977list
4063 Euforbo8.795.619102.46106.38L48.850.9501989list
2357 Phereclos8.9494.62594.9098.45L514.390.9601981list
4709 Ennomos8.591.43380.8580.03L512.280.6901988list
2797 Teucer8.789.430111.14113.99L410.150.9201981list
2920 Automedon8.888.574111.01113.11L410.210.9501981list
15436 Dexius9.187.64685.7178.63L48.970.8701998list
3596 Meriones9.287.38075.0973.28L412.960.8301985list
2893 Peiroos9.2386.88487.4686.76L58.960.9501975list
4086 Podalirius9.185.49586.8985.98L410.430.8701985list | 22 | 0 |
4060 Deipylos9.384.04379.2186.79L49.300.7601987list
1404 Ajax9.383.99081.6996.34L429.380.9601936list
4348 Poulydamas9.582.03270.0887.51L59.910.8401988list
5144 Achates9.080.95891.9189.85L55.960.9201991list
4833 Meges8.980.16587.3389.39L414.250.9401989list
2223 Sarpedon9.4177.48094.63108.21L522.740.8801977list
4489 Dracius9.076.59592.9395.02L412.580.9501988list
2260 Neoptolemus9.3176.43571.6581.28L48.180.9501975list
5254 Ulysses9.276.14778.3480.00L428.720.9701986list
3708 Socus9.375.66179.5976.75L56.550.9801974list
2674 Pandarus9.174.26798.10101.72L58.481.0001982list
3564 Talthybius9.473.73068.9274.11L440.590.9001985list
4834 Thoas9.172.33186.8296.21L418.190.9501989list
7641 Cteatus9.471.83968.9775.28L427.770.9801986list
3540 Protesilaos9.370.22576.8487.66L48.950.9401973list
11395 Iphinous9.868.97764.7167.78L417.38–1998list
4035 Thestor9.668.73368.2366.99L413.470.9701986list
5264 Telephus9.468.47273.2681.38L49.530.9701991list
1868 Thersites9.568.16370.0878.89L410.480.9601960list
9799 Thronium9.668.03364.8772.42L421.520.9101996list
4068 Menestheus9.567.62562.3768.46L414.400.9501973list
23135 Pheidas9.966.23058.2968.50L48.690.8602000list
2456 Palamedes9.365.91691.6699.60L47.240.9201966list
3709 Polypoites9.165.29799.0985.23L410.041.0001985list
1749 Telamon9.564.89881.0669.14L416.980.9701949list
3548 Eurybates9.663.88572.1468.40L48.710.7301973list
4543 Phoinix9.763.83662.7969.54L438.871.2001989list
12444 Prothoon9.863.83564.3162.41L515.82–1996list
4836 Medon9.563.27767.7378.70L49.820.9201989list
16070 Charops9.763.19164.1368.98L520.240.9601999list
15440 Eioneus9.662.51966.4871.88L421.430.9701998list
4715 Medesicaste9.762.09763.9165.93L58.810.8501989list
34746 Thoon9.861.68460.5163.63L519.630.9502001list
38050 Bias9.861.60361.0450.44L418.850.9901998list
5130 Ilioneus9.760.71159.4052.49L514.770.9601989list
5027 Androgeos9.659.78657.86n.a.L411.380.9101988list
6090 Aulis9.459.56874.5381.92L418.480.9801989list
5648 Axius9.759.29563.91n.a.L537.560.9001990list
7119 Hiera9.759.15076.4077.29L44000.9501989list
4805 Asteropaios10.057.64753.1643.44L512.37–1990list
16974 Iphthime9.857.34155.4357.15L478.90.9601998list
4867 Polites9.857.25158.2964.29L511.241.0101989list
2895 Memnon10.056.70655.67n.a.L57.500.7101981list
4708 Polydoros9.954.96455.67n.a.L57.520.9601988list
(21601) 1998 XO8910.054.90955.6756.08L412.650.9701998list
12929 Periboea9.954.07761.0455.34L59.270.8801999list
17492 Hippasos10.053.97555.67n.a.L517.75–1991list
5652 Amphimachus10.153.92153.1652.48L48.371.0501992list
2759 Idomeneus9.953.67661.0152.55L432.380.9101980list
5258 Rhoeo10.253.27550.77n.a.L419.851.0101989list
(12126) 1999 RM1110.153.202n.a.n.a.L5n.a. ?1999list
(15502) 1999 NV2710.053.10055.6750.86L515.130.8751999list
4754 Panthoos10.053.02553.1556.96L527.68–1977list
4832 Palinurus10.052.05853.16n.a.L55.321.0001988list
5126 Achaemenides10.551.92244.2248.57L453.02–1989list
3240 Laocoon10.251.69550.77n.a.L511.310.8801978list
4902 Thessandrus9.851.26361.0471.79L47380.9601989list
11552 Boucolion10.151.13653.1653.91L532.44–1993list
(20729) 1999 XS14310.450.96146.30n.a.L45.721.0001999list
6545 Leitus10.150.95153.16n.a.L416.260.9101986list
4792 Lykaon10.150.87053.16n.a.L540.090.9601988list
21900 Orus10.050.81055.6753.87L413.450.9501999list
1873 Agenor10.150.79953.7654.38L520.60–1971list
5028 Halaesus10.250.77050.77n.a.L424.940.9001988list
2146 Stentor9.950.75558.29n.a.L416.40–1976list
4722 Agelaos10.050.37853.1659.47L518.440.9101977list
5284 Orsilocus10.150.15953.16n.a.L410.310.9701989list
11509 Thersilochos10.149.96053.1656.23L517.37–1990list
5285 Krethon10.149.60658.5352.61L412.041.0901989list
4791 Iphidamas10.149.52857.8559.96L59.701.0301988list
9023 Mnesthus10.149.15150.7760.80L530.66–1988list
5283 Pyrrhus9.748.35664.5869.93L47.320.9501989list
4946 Askalaphus10.248.20952.7166.10L422.730.9401988list | 22 | 1 |
(22149) 2000 WD4910.248.19050.7750.37L47.841.0902000list
(32496) 2000 WX18210.248.01750.7751.63L523.340.9502000list
5120 Bitias10.247.98750.77n.a.L515.210.7801988list
12714 Alkimos10.147.81961.0454.62L428.48–1991list
7352 Hypsenor9.947.73155.67 47.07L56480.8501994list
1870 Glaukos10.647.64942.23n.a.L55.99—1971list
4138 Kalchas10.146.46253.1661.04L429.20.8101973list
(23958) 1998 VD3010.246.00150.7747.91L45620.9901998list
4828 Misenus10.445.95446.30 43.22L512.870.9201988list
4057 Demophon10.145.68353.16n.a.L429.821.0601985list
4501 Eurypylos10.445.52446.30n.a.L46.05–1989list
4007 Euryalos10.345.51548.4853.89L46.39–1973list
5259 Epeigeus10.344.74142.5944.42L418.42–1989list
30705 Idaios10.444.54646.30n.a.L515.74–1977list
16560 Daitor10.743.86151.4243.38L5––1991list
(15977) 1998 MA1110.443.53046.3051.53L52500.9061998list
7543 Prylis10.642.89342.23n.a.L417.80–1973list
4827 Dares10.542.77044.22n.a.L519.00–1988list
1647 Menelaus10.542.71644.22n.a.L417.740.8661957list
(A) Used sources: WISE/NEOWISE catalog (NEOWISE_DIAM_V1 PDS, Grav, 2012); IRAS data (SIMPS v.6 catalog); and Akari catalog (Usui, 2011); RP: rotation period and V–I (color index) taken from the LCDB
Note: missing data was completed with figures from the JPL SBDB (query) and from the LCDB (query form) for the WISE/NEOWISE and SIMPS catalogs, respectively. These figures are given in italics. Also, listing is incomplete above #100.
Notes
1. Lightcurve plots of (15977) 1998 MA11 from Aug 2013 and Dec 2015 by Robert Stephens at the Center for Solar System Studies (U81). Quality code is 1/2- (lightcurve rating at CS3). Summary figures at the LCDB and CS3.
References
1. "15977 (1998 MA11)". Minor Planet Center. Retrieved 1 July 2018.
2. "JPL Small-Body Database Browser: 15977 (1998 MA11)" (2018-04-20 last obs.). Jet Propulsion Laboratory. Retrieved 1 July 2018.
3. "List of Jupiter Trojans". Minor Planet Center. 1 July 2018. Retrieved 1 July 2018.
4. "Asteroid (15977) 1998 MA11 – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 1 July 2018.
5. Grav, T.; Mainzer, A. K.; Bauer, J. M.; Masiero, J. R.; Nugent, C. R. (November 2012). "WISE/NEOWISE Observations of the Jovian Trojan Population: Taxonomy". The Astrophysical Journal. 759 (1): 10. arXiv:1209.1549. Bibcode:2012ApJ...759...49G. doi:10.1088/0004-637X/759/1/49. S2CID 119101711. (online catalog)
6. Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
7. Stephens, Robert D.; Coley, Daniel R.; French, Linda M. (July 2016). "A Report from the L5 Trojan Camp - Lightcurves of Jovian Trojan Asteroids from the Center for Solar System Studies". The Minor Planet Bulletin. 43 (3): 265–270. Bibcode:2016MPBu...43..265S. ISSN 1052-8091.
8. "LCDB Data for (15977)". Asteroid Lightcurve Database (LCDB). Retrieved 1 July 2018.
9. Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited". Astronomy and Astrophysics. 546: 20. arXiv:1209.1896. Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. S2CID 54776793.
10. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 1 July 2018.
11. Stephens, Robert D.; French, Linda M.; Davitt, Chelsea; Coley, Daniel R. (April 2014). "At the Scaean Gates: Observations Jovian Trojan Asteroids, July- December 2013". The Minor Planet Bulletin. 41 (2): 95–100. Bibcode:2014MPBu...41...95S. ISSN 1052-8091.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• Asteroid (15977) 1998 MA11 at the Small Bodies Data Ferret
• (15977) 1998 MA11 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (15977) 1998 MA11 at the JPL Small-Body Database
Minor planets navigator
• (15977) 1998 MA11
Small Solar System bodies
Minor planets
• Designation
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• List
• Moon
• Meanings of names
Asteroid
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• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
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• Cosmic dust
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• JPL SBDB
• MPC | 22 | 2 |
(159857) 2004 LJ1
(159857) 2004 LJ1, provisional designation 2004 LJ1, is an asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 3 kilometers in diameter. The asteroid was discovered on 10 June 2004, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [2] It is one of the largest potentially hazardous asteroids known to exist. [8]
(159857) 2004 LJ1
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date10 June 2004
Designations
MPC designation
(159857) 2004 LJ1
Alternative designations
2004 LJ1
Minor planet category
Apollo · NEO · PHA[1][2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc22.29 yr (8,141 days)
Aphelion3.6072 AU
Perihelion0.9203 AU
Semi-major axis
2.2637 AU
Eccentricity0.5935
Orbital period (sidereal)
3.41 yr (1,244 days)
Mean anomaly
286.61°
Mean motion
0° 17m 21.84s / day
Inclination23.140°
Longitude of ascending node
235.58°
Argument of perihelion
139.97°
Earth MOID0.0168 AU · 6.5 LD
Physical characteristics
Mean diameter
2.47 km (calculated)[3]
3.070±1.324 km[4]
Synodic rotation period
2.661±0.001 h[5][lower-alpha 1]
2.7247±0.0002 h[6]
2.76 h[lower-alpha 2]
Geometric albedo
0.130±0.158[4]
0.20 (assumed)[3]
Spectral type
S (assumed)[3]
Absolute magnitude (H)
15.11±0.94[7] · 15.4[1][3][4]
Orbit and classification
2004 LJ1 is a member of the dynamical Apollo group,[1][2] which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects.
The body orbits the Sun at a distance of 0.9–3.6 AU once every 3 years and 5 months (1,244 days; semi-major axis of 2.26 AU). Its orbit has an eccentricity of 0.59 and an inclination of 23° with respect to the ecliptic. [1] Its observation arc begins with a precovery from the Digitized Sky Survey taken at the Siding Spring Observatory, Australia, in February 1995, more than 9 years prior to its official discovery observation at Socorro. [2]
Close approaches
With an absolute magnitude of at least 15.4, 2004 LJ1 is one of the brightest and presumably largest known potentially hazardous asteroid (see PHA-list). [8] It has an Earth minimum orbital intersection distance of 0.0168 AU (2,510,000 km), which translates into 6.5 lunar distances (LD). [1] On 16 November 2038, this asteroid will make its closest near-Earth encounter at a nominal distance of 0.0198 AU (7.7 LD). [1] It is also classified as a Mars-crosser, crossing the orbit of the Red Planet at 1.66 AU.
Chronology of close approaches of large near-Earth objects since 1981 (A)
PHA Date Approach distance in lunar distances Abs. mag
(H) Diameter (C)
(m) Ref (D)
Nominal (B) Minimum Maximum
(143651) 2003 QO1041981-05-182.7612.7602.76116.01333–4306data
2014 LJ211989-08-017.0346.8437.22416.01333–4306data
4179 Toutatis1992-12-089.3999.3999.39915.302440–2450data
4179 Toutatis2004-09-294.0314.0314.03115.302440–2450data
(159857) 2004 LJ12038-11-167.7197.7197.71915.41746–4394data
(4953) 1990 MU2058-06-058.9868.9848.98814.13199–10329data
4179 Toutatis2069-11-057.7257.7247.72515.302440–2450data
(52768) 1998 OR22079-04-164.6114.6114.61215.81462–4721data
(415029) 2011 UL212089-06-256.9366.9356.93815.71531–4944data
3200 Phaethon2093-12-147.7147.7097.71814.64900–5300data
(52768) 1998 OR22127-04-166.5366.5106.56315.81462–4721data
(A) This list includes near-Earth approaches of less than 10 lunar distances (LD) of objects with H brighter than 16.
(B) Nominal geocentric distance from the center of Earth to the center of the object (Earth has a radius of approximately 6,400 km).
(C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
(D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
(E) Color codes: unobserved at close approach observed during close approach upcoming approaches
Physical characteristics
2004 LJ1 is an assumed stony S-type asteroid. [3]
Rotation period
Three rotational lightcurves of 2004 LJ1 have been obtained from photometric observations by Johanna Torppa, Adrián Galád and Brian Warner since 2004. [5][6][lower-alpha 1][lower-alpha 2] Lightcurve analysis gave a consolidated rotation period of 2.7247 hours with a brightness amplitude between 0.15 and 0.59 magnitude (U=3). [3]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2004 LJ1 measures 3.07 kilometers in diameter and its surface has an albedo of 0.13. [4] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.47 kilometers, based on an absolute magnitude of 15.4. [3]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 June 2007. [9] As of 2018, it has not been named. [2]
Notes
1. Lightcurve plot of (159857) 2004 LJ1 from June to July 2014, by B. D. Warner at the CS3–Palmer Divide Station in California (U82). Quality code of 2. Summary figures at the LCDB and CS3 website.
2. Torppa (2011) web: Undated observation. Rotation period 2.76 hours with a brightness amplitude of 0.5 mag. Quality Code of 2. Summary figures at the LCDB
References
1. "JPL Small-Body Database Browser: 159857 (2004 LJ1)" (2017-05-19 last obs.). Jet Propulsion Laboratory. Retrieved 18 January 2018.
2. "159857 (2004 LJ1)". Minor Planet Center. Retrieved 18 January 2018.
3. "LCDB Data for (159857)". Asteroid Lightcurve Database (LCDB). Retrieved 18 January 2018.
4. Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 18 January 2018.
5. | 23 | 0 |
Warner, Brian D. (January 2015). "Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2014 June-October". The Minor Planet Bulletin. 42 (1): 41–53. Bibcode:2015MPBu...42...41W. ISSN 1052-8091. Retrieved 18 January 2018.
6. Galád, A.; Pravec, P.; Kusnirák, P.; Gajdos, S.; Kornos, L.; Világi, J. (October 2005). "Joint Lightcurve Observations of 10 Near-Earth Asteroids from Modra and ONDREJOV". Earth. 97 (1–2): 147–163. Bibcode:2005EM&P...97..147G. doi:10.1007/s11038-006-9066-x. Retrieved 18 January 2018.
7. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 18 January 2018.
8. "List of the Potentially Hazardous Asteroids (PHAs)". Minor Planet Center. Retrieved 18 January 2018.
9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• (159857) 2004 LJ1 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (159857) 2004 LJ1 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary
• (159857) 2004 LJ1 at the JPL Small-Body Database
Minor planets navigator
• (159857) 2004 LJ1
Small Solar System bodies
Minor planets
• Designation
• Groups
• List
• Moon
• Meanings of names
Asteroid
• Active
• Aten asteroid
• Asteroid belt
• Family
• Jupiter trojan
• Near-Earth
• Spectral types
Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
• Extinct
• Great
• Halley-type
• Hyperbolic
• Long-period
• Lost
• Near-parabolic
• Periodic
• Sungrazing
Other
• Cosmic dust
• Meteoroids
• Space debris
Authority control databases
• JPL SBDB
• MPC | 23 | 1 |
(163243) 2002 FB3
(163243) 2002 FB3, provisional designation 2002 FB3, is a stony asteroid on an eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Athen group, approximately 1.6 kilometers (1 mile) in diameter. It was discovered on 18 March 2002, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [1] The Q-type asteroid has a rotation period of 6.2 hours. [3]
(163243) 2002 FB3
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date18 March 2002
Designations
MPC designation
(163243) 2002 FB3
Alternative designations
2002 FB3
Minor planet category
Aten · NEO · PHA[1][2]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc16.07 yr (5,869 d)
Aphelion1.2198 AU
Perihelion0.3033 AU
Semi-major axis
0.7616 AU
Eccentricity0.6017
Orbital period (sidereal)
243 days
Mean anomaly
150.26°
Mean motion
1° 28m 58.8s / day
Inclination20.278°
Longitude of ascending node
203.60°
Argument of perihelion
148.31°
Earth MOID0.0034 AU (1.3246 LD)
Physical characteristics
Mean diameter
1.49 km (calculated)[3]
1.552±0.013 km[4]
1.663±0.285 km[5]
1.682±0.013 km[6]
Synodic rotation period
6.231±0.001 h[7]
Geometric albedo
0.1426±0.1478[5]
0.172±0.041[6]
0.202±0.046[4]
0.20 (assumed)[3]
Spectral type
Q[3][8]
Absolute magnitude (H)
16.4[2][4]
16.50[3][5]
Orbit and classification
2002 FB3 is a member of the Athen group of asteroids. It orbits the Sun at a distance of 0.3–1.2 AU once every 8 months (243 days; semi-major axis of 0.76 AU). Its orbit has an eccentricity of 0.60 and an inclination of 20° with respect to the ecliptic. [2] The body's observation arc begins with its official discovery observation at Socorro. [1]
Close approaches
The asteroid has an Earth minimum orbital intersection distance of 0.0034 AU (509,000 km; 316,000 mi), which corresponds to 1.3 lunar distances and makes it a potentially hazardous asteroid due to its sufficiently large size. [2]
History of close approaches of large near-Earth objects since 1908 (A)
PHA Date Approach distance (lunar dist.) Abs.
mag
(H) Diameter (C)
(m) Ref (D)
Nomi-
nal(B) Mini-
mum Maxi-
mum
(33342) 1998 WT241908-12-163.5423.5373.54717.9556–1795data
(458732) 2011 MD51918-09-170.9110.9090.91317.9556–1795data
(7482) 1994 PC11933-01-172.9272.9272.92816.8749–1357data
69230 Hermes1937-10-301.9261.9261.92717.5668–2158data
69230 Hermes1942-04-261.6511.6511.65117.5668–2158data
(137108) 1999 AN101946-08-072.4322.4292.43517.9556–1795data
(33342) 1998 WT241956-12-163.5233.5233.52317.9556–1795data
(163243) 2002 FB31961-04-124.9034.9004.90616.41669–1695data
(192642) 1999 RD321969-08-273.6273.6253.63016.31161–3750data
(143651) 2003 QO1041981-05-182.7612.7602.76116.01333–4306data
2017 CH11992-06-054.6913.3916.03717.9556–1795data
(170086) 2002 XR141995-06-244.2594.2594.26018.0531–1714data
(33342) 1998 WT242001-12-164.8594.8594.85917.9556–1795data
4179 Toutatis2004-09-294.0314.0314.03115.32440–2450data
2014 JO252017-04-194.5734.5734.57317.8582–1879data
(137108) 1999 AN102027-08-071.0141.0101.01917.9556–1795data
(35396) 1997 XF112028-10-262.4172.4172.41816.9881–2845data
(154276) 2002 SY502071-10-303.4153.4123.41817.6714–1406data
(164121) 2003 YT12073-04-294.4094.4094.40916.21167–2267data
(385343) 2002 LV2076-08-044.1844.1834.18516.61011–3266data
(52768) 1998 OR22079-04-164.6114.6114.61215.81462–4721data
(33342) 1998 WT242099-12-184.9194.9194.91917.9556–1795data
(85182) 1991 AQ2130-01-274.1404.1394.14117.11100data
314082 Dryope2186-07-163.7092.9964.78617.5668–2158data
(137126) 1999 CF92192-08-214.9704.9674.97318.0531–1714data
(290772) 2005 VC2198-05-051.9511.7912.13417.6638–2061data
(A) List includes near-Earth approaches of less than 5 lunar distances (LD) of objects with H brighter than 18.
(B) Nominal geocentric distance from the Earth's center to the object's center (Earth radius≈0.017 LD).
(C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
(D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
(E) Color codes: unobserved at close approach observed during close approach upcoming approaches
Physical characteristics
2003 QO104 has been characterized as an uncommon Q-type asteroid, that fall into the larger stony S-complex. [3][8]
Rotation period
In March 2016, a rotational lightcurve of this asteroid was obtained from photometric observations. Lightcurve analysis gave a rotation period of 6.231 hours with a brightness amplitude of 0.19 magnitude (U=2). [7]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures between 1.552 and 1.682 kilometers in diameter and its surface has an albedo between 0.1426 and 0.202. [4][5][6]
The Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 and calculates a diameter of 1.49 kilometers based on an absolute magnitude of 16.5. [3]
Naming
This minor planet was numbered by the MPC on 26 September 2007 (M.P.C. 60678). [9] As of 2018, it has not been named. [1]
References
1. "163243 (2002 FB3)". Minor Planet Center. | 24 | 0 |
Retrieved 20 April 2018.
2. "JPL Small-Body Database Browser: 163243 (2002 FB3)" (2018-04-12 last obs.). Jet Propulsion Laboratory. Retrieved 20 April 2018.
3. "LCDB Data for (163243)". Asteroid Lightcurve Database (LCDB). Retrieved 20 April 2018.
4. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID 118700974.
5. Masiero, Joseph R.; Nugent, C.; Mainzer, A. K.; Wright, E. L.; Bauer, J. M.; Cutri, R. M.; et al. (October 2017). "NEOWISE Reactivation Mission Year Three: Asteroid Diameters and Albedos". The Astronomical Journal. 154 (4): 10. arXiv:1708.09504. Bibcode:2017AJ....154..168M. doi:10.3847/1538-3881/aa89ec. S2CID 45334910.
6. Mainzer, A.; Grav, T.; Bauer, J.; Masiero, J.; McMillan, R. S.; Cutri, R. M.; et al. (December 2011). "NEOWISE Observations of Near-Earth Objects: Preliminary Results". The Astrophysical Journal. 743 (2): 17. arXiv:1109.6400. Bibcode:2011ApJ...743..156M. doi:10.1088/0004-637X/743/2/156. S2CID 239991.
7. Monteiro, Filipe; Silva, Jose Sergio; Lazzaro, Daniela; Arcoverde, Plicida; Medeiros, Hissa; Souza, Roberto; et al. (January 2017). "Lightcurve Analysis for Ten Near-Earth Asteroids". The Minor Planet Bulletin. 44 (1): 20–22. Bibcode:2017MPBu...44...20M. ISSN 1052-8091.
8. Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbó, Marco; Hora, Joseph L.; Mueller, Michael (January 2014). "Physical characterization of Warm Spitzer-observed near-Earth objects". Icarus. 228: 217–246. arXiv:1310.2000. Bibcode:2014Icar..228..217T. doi:10.1016/j.icarus.2013.10.004. S2CID 119278697.
9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 April 2018.
External links
• List Of Aten Minor Planets (by designation), Minor Planet Center
• List of the Potentially Hazardous Asteroids (PHAs), Minor Planet Center
• PHA Close Approaches To The Earth, Minor Planet Center
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• (163243) 2002 FB3 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (163243) 2002 FB3 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary
• (163243) 2002 FB3 at the JPL Small-Body Database
Minor planets navigator
• (163243) 2002 FB3
Small Solar System bodies
Minor planets
• Designation
• Groups
• List
• Moon
• Meanings of names
Asteroid
• Active
• Aten asteroid
• Asteroid belt
• Family
• Jupiter trojan
• Near-Earth
• Spectral types
Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
• Extinct
• Great
• Halley-type
• Hyperbolic
• Long-period
• Lost
• Near-parabolic
• Periodic
• Sungrazing
Other
• Cosmic dust
• Meteoroids
• Space debris
Authority control databases
• JPL SBDB
• MPC | 24 | 1 |
163693 Atira
163693 Atira (/əˈtɪrə/; provisional designation 2003 CP20) is a stony asteroid, dwelling in the interior of Earth's orbit. It is classified as a near-Earth object. Atira is a binary asteroid, a system of two asteroids orbiting their common barycenter. The primary component with a diameter of approximately 4.8 kilometers (3 miles)[7] is orbited by a minor-planet moon that measures about 1 km (0.6 mi). [4] Atira was discovered on 11 February 2003, by astronomers with the Lincoln Near-Earth Asteroid Research at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [1][10]
163693 Atira
Arecibo discovery image of orbiting satellite taken on 20 January 2017
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab ETS
Discovery date11 February 2003
Designations
MPC designation
(163693) Atira
Pronunciation/əˈtɪrə/
Pawnee: [ətíɾəʔ]
Named after
Atíraʼ "my/our mother"[1] (Pawnee epithet of the earth goddess)[2]
Alternative designations
2003 CP20
Minor planet category
• NEO
• Atira[1][3]
• Venus-crosser
Symbol
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc14.21 yr (5,192 d)
Aphelion0.9798 AU
Perihelion0.5024 AU
Semi-major axis
0.7411 AU
Eccentricity0.3221
Orbital period (sidereal)
233 days
Mean anomaly
30.769°
Mean motion
1° 32m 41.64s / day
Inclination25.618°
Longitude of ascending node
103.90°
Argument of perihelion
252.93°
Known satellites1[4][5][6][7]
• D: 1.0±0.3 km
• P: 15.5 h
• Type: synchronous
Earth MOID0.2076 AU (80.88 LD)
Physical characteristics
Mean diameter
4.8±0.5 km[4][5][6][7]
Synodic rotation period
3.3984±0.0006 h[7]
Pole ecliptic latitude
−50°[8]
Pole ecliptic longitude
192°[8]
Geometric albedo
0.0231 (derived)[7]
Spectral type
S (assumed)[7]
Absolute magnitude (H)
16.3[3][7][9]
It is the namesake and the first numbered body of the Atira asteroids, a new subclass of near-Earth asteroids, which have their orbits entirely within that of Earth and are therefore alternatively called Interior-Earth Objects (IEO). [3][11][12] As of 2019, there are only 36 known members of the Atira group of asteroids. [13] Atiras are similar to the larger group of Aten asteroids, as both are near-Earth objects and both have a semi-major axis smaller than that of Earth (< 1.0 AU). However, and contrary to Aten asteroids, the aphelion for Atiras is always smaller than Earth's perihelion (< 0.983 AU),[14] which means that they do not approach Earth as close as Atens do in general. Atira has an Earth minimum orbit intersection distance of 0.2059 AU (30,800,000 km) or approximately 80.1 lunar distances. [3]
Physical properties
Atira is a S-type asteroid and orbits the Sun at a distance of 0.5–1.0 AU once every 8 months (233 days). Its orbit has an eccentricity of 0.32 and an inclination of 26° with respect to the ecliptic. [3] With a perihelion of 0.50 AU the body also classifies as a Venus-crosser – as Venus orbits the Sun at a distance of 0.72–0.73 AU – but does not get as close to the Sun as Mercury (which orbits between 0.31 and 0.47 AU). As no precoveries were found, Atira's observation arc begins with its discovery observation in 2003. [1] It has a rotation period of 3.3984 hours with a brightness variation of 0.36 magnitude (U=2) and a very low albedo of 0.0231. [7]
With a diameter of 4.8 kilometers, Atira is one of the largest Near-Earth objects. Early estimates of its size ranged from 1 to 2 kilometers,[10] but those were based on an assumed higher albedo of 0.20. Its larger size and low albedo were discovered when Atira was imaged by radar in early 2017. [4] These radar images also revealed that Atira is a binary asteroid.
Binary system
Atira came within 0.207 AU (31,000,000 km) from Earth in January 2017, the closest since its discovery in 2003. [3] This provided an opportunity to study the asteroid by radar. Images taken at Arecibo Observatory on 20 January 2017 revealed that Atira is a synchronous binary asteroid with a minor-planet moon, S/2017 (163693) 1, in orbit. [4][6] The primary with a diameter of 4.8±0.5 km is possibly elongated and very angular in shape. The secondary is tidally locked and has a diameter of 1.0±0.3 km. Additional images taken on 23 January 2017 showed that the two components are orbiting each other at a distance of about 6 km with an orbital period of 15.5 hours. [4][5]
Name
Because the first known object in a new class of asteroids will become the name of the new class, due consideration was given to the name for (163693). The other classes of near-Earth asteroids, Amors, Apollos, and Atens, are named after a Roman, Greek, and Egyptian god respectively, each of which begins with the letter 'A'. Atira follows this pattern, being named after Atiraʼ [ətíɾəʔ], an epithet of the Earth goddess of the Native American Pawnee people. Atiraʼ is the wife of the creator god, Tirawa, and goddess of Earth and the evening star. [1][15] The official naming citation was published by the Minor Planet Center on 22 January 2008 (M.P.C. 61768). [16]
See also
• 594913 ꞌAylóꞌchaxnim
References
1. "163693 Atira (2003 CP20)". Minor Planet Center. Retrieved 21 April 2018.
2. Douglas Parks & Lula Pratt, A Dictionary of Skiri Pawnee, University of Nebraska Press, 2008. atira, AISRI Dictionary Database Search, Indiana University.
3. "JPL Small-Body Database Browser: 163693 Atira (2003 CP20)" (2017-04-30 last obs.). Jet Propulsion Laboratory. Retrieved 21 April 2018.
4. "Discovery Announcement of Binary System (163693) Atira". Arecibo Observatory. Retrieved 29 May 2017.
5. Johnston, Wm. Robert (19 February 2017). "Asteroids with Satellites Database – (163693) Atira". Johnston's Archive. Retrieved 21 April 2018.
6. Rivera-Valentin, E. G.; Taylor, P. A.; Virkki, A.; Aponte-Hernandez, B. (January 2017). "(163693) Atira". Central Bureau Electronic Telegrams. 4347: 1. Bibcode:2017CBET.4347....1R.
7. "LCDB Data for (163693) Atira". Asteroid Lightcurve Database (LCDB). Retrieved 29 May 2017.
8. Deleon, Aaron P.; Becker, Tracy M.; Marshall, Sean E.; Pravec, Petr; Hornoch, Kamil; Kučáková, Hana; et al. (March 2023). Characterization of Asteroid (163693) Atira with Arecibo Radar and Multi-Epoch Photometric Observations (PDF). 54th Lunar and Planetary Science Conference 2023. Lunar and Planetary Institute. Retrieved 4 February 2023.
9. "(163693) Atira – PHYSICAL INFORMATION". NEODyS: Near Earth Objects – Dynamic Site. Retrieved 29 May 2017. | 25 | 0 |
10. "Lincoln Laboratory discovers inner Earth orbit asteroids". Lincoln Observatory, MIT. Archived from the original on 10 October 2015. Retrieved 29 May 2017.
11. Wm. Robert Johnston (24 August 2006). "Names of Solar System objects and features". Retrieved 11 November 2016.
12. Shoemaker, E. M. (December 1982). "Asteroid and comet bombardment of the earth". Annual Review of Earth and Planetary Sciences. 11: 461–494. Bibcode:1983AREPS..11..461S. doi:10.1146/annurev.ea.11.050183.002333.
13. de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 August 2019). "Understanding the evolution of Atira-class asteroid 2019 AQ3, a major step towards the future discovery of the Vatira population". Monthly Notices of the Royal Astronomical Society. 487 (2): 2742–2752. arXiv:1905.08695. Bibcode:2019MNRAS.487.2742D. doi:10.1093/mnras/stz1437.
14. "NEO Groups". Jet Propulsion Laboratory. Archived from the original on 2 February 2002. Retrieved 9 December 2015.
15. "Ancient Gods & Goddesses". www.godfinder.org. Retrieved 29 May 2017.
16. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 21 April 2018.
External links
• Photo at klet.org
• Facts Sheet (163693) Atira, European Asteroid Research Node (EARN)
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids with Satellites, Robert Johnston, johnstonsarchive.net
• Discovery Circumstances – Numbered Minor Planets (160001)–(165000)
• 163693 Atira at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• 163693 Atira at the JPL Small-Body Database
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• 163693 Atira
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(16882) 1998 BO13
(16882) 1998 BO13 (provisional designation 1998 BO13) is a dark Zhongguo asteroid from the background population in the outermost region of the asteroid belt, approximately 10 kilometers (6 miles) in diameter. It was discovered on 24 January 1998, by astronomers with the Lincoln Near-Earth Asteroid Research at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [1]
(16882) 1998 BO13
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date24 January 1998
Designations
MPC designation
(16882) 1998 BO13
Alternative designations
1998 BO13 · 1999 JC21
Minor planet category
main-belt[1] · (outer)[2]
Zhongguo[3] · 2:1 res[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc20.49 yr (7,483 d)
Aphelion3.9425 AU
Perihelion2.6761 AU
Semi-major axis
3.3093 AU
Eccentricity0.1913
Orbital period (sidereal)
6.02 yr (2,199 d)
Mean anomaly
57.356°
Mean motion
0° 9m 49.32s / day
Inclination0.5370°
Longitude of ascending node
339.83°
Argument of perihelion
225.85°
Physical characteristics
Mean diameter
9.827±0.226 km[5]
Geometric albedo
0.061±0.010[5]
Absolute magnitude (H)
13.5[2]
Orbit and classification
1998 BO13 is a non-family asteroid from the main belt's background population,[6] and a member of the small group of Zhongguo asteroids,[3] located in the Hecuba gap and locked in a 2:1 mean-motion resonance with the gas giant Jupiter. Contrary to the nearby Griqua group, the orbits of the Zhongguos are stable over half a billion years. [3] According to Milani and Knežević, this asteroid is a core member of the unnamed asteroid family formed by the Zhongguo asteroid (11097) 1994 UD1. [4]
It orbits the Sun in the outer main-belt at a distance of 2.7–3.9 AU once every 6.02 years (2,199 days; semi-major axis of 3.31 AU). Its orbit has an eccentricity of 0.19 and an inclination of 1° with respect to the ecliptic. [2]
The body's observation arc begins with a precovery taken by Spacewatch in November 1996, or 14 months prior to its official discovery observation at Socorro. [1]
Physical characteristics
1998 BO13 has an absolute magnitude of 13.5. [2] As of 2018, no rotational lightcurve for this asteroid has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown. [2]
Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, measures 9.827 kilometers in diameter and its surface has an albedo of 0.061,[5] which is rather typical for the abundant carbonaceous C-type asteroids in the outer main-belt.
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 September 2000, after its orbit had sufficiently been secured (M.P.C. 41165). [7] As of 2018, it has not been named. [1]
References
1. "16882 (1998 BO13)". Minor Planet Center. Retrieved 26 April 2018.
2. "JPL Small-Body Database Browser: 16882 (1998 BO13)" (2017-05-03 last obs.). Jet Propulsion Laboratory. Retrieved 26 April 2018.
3. Roig, F.; Nesvorný, D.; Ferraz-Mello, S. (September 2002). "Asteroids in the 2 : 1 resonance with Jupiter: dynamics and size distribution [ Erratum: 2002MNRAS.336.1391R ]". Monthly Notices of the Royal Astronomical Society. 335 (2): 417–431. Bibcode:2002MNRAS.335..417R. doi:10.1046/j.1365-8711.2002.05635.x. Retrieved 26 April 2018.
4. "Asteroid (16882) 1998 BO13 – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. S2CID 118745497. Retrieved 26 April 2018.
6. "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Archived from the original on 2 August 2017. Retrieved 26 April 2018.
7. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 26 April 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (15001)-(20000) – Minor Planet Center
• (16882) 1998 BO13 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (16882) 1998 BO13 at the JPL Small-Body Database
Minor planets navigator
• (16882) 1998 BO13
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(16960) 1998 QS52
(16960) 1998 QS52 (provisional designation 1998 QS52) is a stony asteroid on a highly eccentric orbit, classified as near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 4.1 kilometers (2.5 mi) in diameter. It was discovered on 25 August 1998, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. [2] This asteroid is one of the largest potentially hazardous asteroid known to exist. [8]
(16960) 1998 QS52
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date25 August 1998
Designations
MPC designation
(16960) 1998 QS52
Alternative designations
1998 QS52
Minor planet category
Apollo · NEO · PHA[1][2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc34.36 yr (12,551 days)
Aphelion4.0928 AU
Perihelion0.3133 AU
Semi-major axis
2.2030 AU
Eccentricity0.8578
Orbital period (sidereal)
3.27 yr (1,194 days)
Mean anomaly
244.09°
Mean motion
0° 18m 5.04s / day
Inclination17.546°
Longitude of ascending node
260.48°
Argument of perihelion
242.95°
Earth MOID0.0144 AU (5.6 LD)
Physical characteristics
Mean diameter
4.10 km (calculated)[3]
Synodic rotation period
2.900±0.001 h (alternative)[4][lower-alpha 1]
5.789±0.001 h[3]
5.8±0.1 h[5]
Geometric albedo
0.20 (assumed)[3]
Spectral type
SMASS = Sq[1] · Sr[6]
Absolute magnitude (H)
14.3[1][3] · 14.79±0.23[7]
Orbit and classification
1998 QS52 is a member of the dynamical Apollo group,[1][2] which are Earth-crossing asteroids. Apollo asteroids are the largest subgroup of near-Earth objects. It orbits the Sun at a distance of 0.31–4.1 AU once every 3 years and 3 months (1,194 days; semi-major axis of 2.20 AU). Its orbit has an exceptionally high eccentricity of 0.86 and an inclination of 18° with respect to the ecliptic. [1]
The body's observation arc begins with a precovery taken at the Siding Spring Observatory in June 1983, more than 15 years prior to its official discovery observation at Socorro. [2]
Close approaches
With an absolute magnitude of 14.3, 1998 QS52 is one of the brightest and largest known potentially hazardous asteroid (see PHA-list). [8] It has an Earth minimum orbital intersection distance of 0.0144 AU (2,150,000 km), which corresponds to 5.6 lunar distances. [1] Its eccentric orbit leads to close approaches with Mercury and Venus and carries it beyond the asteroid belt but not as far as to the orbit of Jupiter (>4.9 AU). It is therefore also a Venus- and Mars-crossing asteroid. [1]
Physical characteristics
In the SMASS classification, 1998 QS52 is a Sq-subtype, that transitions between the stony S- and Q-type asteroids. [1] Observers at the NASA Infrared Telescope Facility have also characterized this body as an Sr-type, which transitions to the rare R-type asteroids. [6]
Rotation period
In 2008, two rotational lightcurves of 1998 QS52 were obtained independently from photometric observations by Brian Warner at the Palmer Divide Observatory and by Brian Skiff during the Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) . Lightcurve analysis gave a rotation period of 5.789 and 5.8 hours with a brightness amplitude of 0.24 and 1.4 magnitude, respectively (U=2/2). [3][5] An alternative period solution of 2.9 hours – or half of the above period – is also possible, though considered less likely by Warner. [4][lower-alpha 1]
Diameter and albedo
1998 QS52 has not been observed by any of the space-based surveys such as IRAS, Akari or the Wide-field Infrared Survey Explorer. The Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 for its surface, and calculates a diameter of 4.10 kilometers based on an absolute magnitude of 14.3. [3]
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 September 2000. [9] As of 2018, it has not been named. [2]
Notes
1. Lightcurve plot of (16960) 1998 QS52: alternative period solution of 2.900±0.001 hours with a brightness amplitude of 0.24±0.02 mag. Quality Code of 2. Summary figures at the LCDB
References
1. "JPL Small-Body Database Browser: 16960 (1998 QS52)" (2017-10-24 last obs.). Jet Propulsion Laboratory. Retrieved 17 January 2018.
2. "16960 (1998 QS52)". Minor Planet Center. Retrieved 17 January 2018.
3. "LCDB Data for (16960)". Asteroid Lightcurve Database (LCDB). Retrieved 17 January 2018.
4. Warner, Brian D. (January 2009). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2008 May - September". The Minor Planet Bulletin. 36 (1): 7–13. Bibcode:2009MPBu...36....7W. ISSN 1052-8091. Retrieved 17 January 2018.
5. Skiff, Brian A.; Bowell, Edward; Koehn, Bruce W.; Sanborn, Jason J.; McLelland, Kyle P.; Warner, Brian D. (July 2012). "Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS) - 2008 May through 2008 December". The Minor Planet Bulletin. 39 (3): 111–130. Bibcode:2012MPBu...39..111S. ISSN 1052-8091. Retrieved 17 January 2018.
6. Popescu, M.; Birlan, M.; Binzel, R.; Vernazza, P.; Barucci, A.; Nedelcu, D. A.; et al. (November 2011). "Spectral properties of eight near-Earth asteroids". Astronomy and Astrophysics. 535: 15. Bibcode:2011A&A...535A..15P. doi:10.1051/0004-6361/201117118. Retrieved 17 January 2018.
7. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339. Retrieved 17 January 2018.
8. "List of the Potentially Hazardous Asteroids (PHAs)". Minor Planet Center. Retrieved 18 January 2018.
9. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• (16960) 1998 QS52 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (16960) 1998 QS52 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary | 27 | 0 |
• (16960) 1998 QS52 at the JPL Small-Body Database
Minor planets navigator
• (16960) 1998 QS52
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Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
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17 Thetis
Thetis, minor planet designation 17 Thetis, is a stony asteroid from the inner regions of the asteroid belt, approximately 90 kilometers in diameter. It was discovered on 17 April 1852, by German astronomer Robert Luther at Bilk Observatory in Düsseldorf, Germany who deferred to Friedrich Wilhelm August Argelander the naming his first asteroid discovery after Thetis from Greek mythology. [3][4] Its historical symbol was a dolphin and a star; it is in the pipeline for Unicode 17.0 as U+1CECA (). [12][13]
17 Thetis
Star field showing asteroid Thetis in the center
Discovery[1]
Discovered byR. Luther
Discovery siteDüsseldorf-Bilk Obs.
Discovery date17 April 1852
Designations
MPC designation
(17) Thetis
Pronunciation/ˈθiːtɪs/[2]
Named after
Thetis (Greek mythology)[3]
Alternative designations
1954 SO1 · A913 CA
A916 YF
Minor planet category
main-belt[4] · (inner)
AdjectivesThetidian /θɛˈtɪdiən/[5]
Symbol (historical)
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc164.55 yr (60,102 days)
Aphelion2.7987 AU
Perihelion2.1436 AU
Semi-major axis
2.4712 AU
Eccentricity0.1325
Orbital period (sidereal)
3.88 yr (1,419 days)
Average orbital speed
18.87 km/s
Mean anomaly
100.44°
Mean motion
0° 15m 13.32s / day
Inclination5.5902°
Longitude of ascending node
125.56°
Argument of perihelion
136.10°
Physical characteristics
Dimensions84.899±2.027[6]
90±3.7km (IRAS)[7]
93.335±2.627[8]
Mass1.23×1018 kg[9][lower-alpha 1]
Mean density
3.21±0.92 g/cm3[9]
Synodic rotation period
12.27048±0.00001[10][11]
Geometric albedo
0.193±0.028[6]
Spectral type
B–V = 0.829[1]
U–B = 0.438[1]
S (Tholen)[1]
Sl (SMASS)[1] · S[10]
Absolute magnitude (H)
7.76[1][7][8] · 7.85[11]
Description
The asteroid orbits the Sun at a distance of 2.1–2.8 AU once every 3 years and 11 months (1,419 days). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic. [1]
The spectrum of this object indicates that it is an S-type asteroid with both low and high calcium forms of pyroxene on the surface, along with less than 20% olivine. The high-calcium form of pyroxene forms 40% or more of the total pyroxene present, indicating a history of igneous rock deposits. This suggests that the asteroid underwent differentiation by melting, creating a surface of basalt rock. [14]
The mass of Thetis has been calculated from perturbations by 4 Vesta and 11 Parthenope. In 2007, Baer and Chesley calculated Thetis to have a mass of 1.23×1018 kg[lower-alpha 1] with a density of 3.21 g/cm3. [9]
One Thetidian stellar occultation was observed from Oregon in 1999. However, the event was not timed.
This minor planet was named after Thetis, the mother of Achilles in Greek mythology. [3]
Notes
1. Mass of Thetis = (6.17±0.64)×10−13 M☉
References
1. "JPL Small-Body Database Browser: 17 Thetis" (2016-11-11 last obs.). Jet Propulsion Laboratory. Retrieved 24 March 2017.
2. Noah Webster (1884) A Practical Dictionary of the English Language
3. Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (17) Thetis. Springer Berlin Heidelberg. p. 17. doi:10.1007/978-3-540-29925-7_18. ISBN 978-3-540-00238-3.
4. "17 Thetis". Minor Planet Center. Retrieved 24 March 2017.
5. Herbert (1828) Nimrod: a discourse on certain passages of history and fable, vol. 2
6. Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121.
7. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 30 October 2019.
8. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
9. Baer, James; Chesley, Steven R. (January 2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris". Celestial Mechanics and Dynamical Astronomy. 100 (1): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8.
10. "LCDB Data for (17) Thetis". Asteroid Lightcurve Database (LCDB). Retrieved 24 March 2017.
11. Michalowski, T.; Velichko, F. P.; Di Martino, M.; Krugly, Yu. N.; Kalashnikov, V. G.; Shevchenko, V. G.; et al. (December 1995). "Models of four asteroids: 17 Thetis, 52 Europa, 532 Herculina, and 704 Interamnia". Icarus. 118 (2): 292–301. Bibcode:1995Icar..118..292M. doi:10.1006/icar.1995.1192.
12. Bala, Gavin Jared; Miller, Kirk (18 September 2023). "Unicode request for historical asteroid symbols" (PDF). unicode.org. Unicode. Retrieved 26 September 2023.
13. Unicode. "Proposed New Characters: The Pipeline". unicode.org. The Unicode Consortium. Retrieved 6 November 2023.
14. Sunshine, Jessica M.; Bus, Schelte J.; McCoy, Timothy J.; Burbine, Thomas H.; Corrigan, Catherine M.; Binzel, Richard P. (August 2004). "High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites". Meteoritics and Planetary Science. 39 (8): 1343–1357. Bibcode:2004M&PS...39.1343S. doi:10.1111/j.1945-5100.2004.tb00950.x.
External links
Wikimedia Commons has media related to 17 Thetis.
• 2011-Apr-22 Occultation (Durech Model) / (2011 Asteroidal Occultation Results for North America)
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine) | 28 | 0 |
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves – (17) Thetis at Observatoire de Genève, Raoul Behrend
• Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
• 17 Thetis at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 17 Thetis at the JPL Small-Body Database
Minor planets navigator
• 16 Psyche
• 17 Thetis
• 18 Melpomene
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• Detached
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Comets
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• Cosmic dust
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• JPL SBDB
• MPC | 28 | 1 |
(17511) 1992 QN
(17511) 1992 QN (provisional designation 1992 QN) is a small, bright Apollo asteroid discovered on August 29, 1992 by American astronomers Eleanor Helin and Jeff Alu at the Palomar Observatory, California, United States. It is a near-Earth asteroid whose orbit crosses that of Mars and Earth (a Mars and Earth-crossing asteroid). On January 18, 1996, it passed Earth at a distance of 0.158848 AU (23.763 million km), and on July 12, 2027, it will pass our planet again at a distance of 0.161858 AU (24.214 million km). [3] (17511) 1992 QN's orbit is similar to that of Apollo asteroid 2010 JG. [4]
(17511) 1992 QN
Discovery[1]
Discovered byEleanor Helin and Jeff Alu
Designations
Alternative designations
1992 QN
Minor planet category
Apollo
Orbital characteristics[2]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc9656 days (26.44 yr)
Aphelion1.61699 AU (241.898 Gm)
Perihelion0.76297 AU (114.139 Gm)
Semi-major axis
1.18998 AU (178.018 Gm)
Eccentricity0.35884
Orbital period (sidereal)
1.3 yr (474.14 d)
Average orbital speed
27.3 km/s
Mean anomaly
235.804°
Mean motion
0° 45m 33.365s / day
Inclination9.58265°
Longitude of ascending node
355.924°
Argument of perihelion
202.359°
Earth MOID0.132266 AU (19.7867 Gm)
Physical characteristics
Synodic rotation period
6 h (0.25 d)
Spectral type
X
Absolute magnitude (H)
17.3
References
1. "Info". JPL Small-Body Database Browser. Retrieved 6 February 2021.
2. "(17511) 1992 QN". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 6 February 2021.
3. "(17511) 1992 QN close approaches". Near Earth Objects. Archived from the original on 2021-12-09. Retrieved 8 February 2021.
4. "2010 JG: Very small Apollo-class Asteroid". Space Reference. Archived from the original on 2021-02-14. Retrieved 8 February 2021.
External links
• NEODyS-2 statistics of (17511) 1992 QN
• JPL Small-Body Database's orbit diagram and statistics of (17511) 1992 QN
Minor planets navigator
• (17511) 1992 QN
Small Solar System bodies
Minor planets
• Designation
• Groups
• List
• Moon
• Meanings of names
Asteroid
• Active
• Aten asteroid
• Asteroid belt
• Family
• Jupiter trojan
• Near-Earth
• Spectral types
Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
• Extinct
• Great
• Halley-type
• Hyperbolic
• Long-period
• Lost
• Near-parabolic
• Periodic
• Sungrazing
Other
• Cosmic dust
• Meteoroids
• Space debris
Authority control databases
• JPL SBDB
• MPC | 29 | 0 |
(177049) 2003 EE16
(177049) 2003 EE16, provisionally known as 2003 EE16, is an Apollo near-Earth asteroid and potentially hazardous object. [2] It was discovered on 8 March 2003 by LPL/Spacewatch II at an apparent magnitude of 20 using a 1.8-meter (71 in) reflecting telescope. [1] It has an estimated diameter of 320 meters (1,050 ft). [3] The asteroid was listed on Sentry Risk Table with a Torino Scale rating of 1 on 2 April 2003. [3]
(177049) 2003 EE16
Discovery[1]
Discovered bySpacewatch
Discovery siteKitt Peak National Obs.
Discovery date8 March 2003
Designations
MPC designation
(177049) 2003 EE16
Minor planet category
NEO · PHA · Apollo[2]
Orbital characteristics[2]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc4429 days (12.13 yr)
Earliest precovery date17 May 2002
Aphelion2.2878 AU (342.25 Gm)
Perihelion0.54666 AU (81.779 Gm)
Semi-major axis
1.4172 AU (212.01 Gm)
Eccentricity0.61427
Orbital period (sidereal)
1.69 yr (616.24 d)
Mean anomaly
296.40°
Mean motion
0° 35m 3.084s / day
Inclination0.64964°
Longitude of ascending node
127.04°
Argument of perihelion
259.67°
Earth MOID9.93475×10−5 AU (1.486217×104 km)
Physical characteristics
Mean diameter
0.320 km[3]
Mass5.1×1010 kg (assumed)
Absolute magnitude (H)
19.7[2]
Description
Many of the virtual impactors were located near the nominal orbital solution and the asteroid has a low inclination relative to Earth's orbit. [4] Observation by the Very Large Telescope (VLT) 8 meter facilities on 22 May and 19 June 2003 when 2003 EE16 was very dim with an apparent magnitude between 24–25[note 1] refined the orbit. [4] It was removed from the Sentry Risk Table on 28 May 2003. [5]
2003 EE16 has the smallest Earth Minimum orbit intersection distance (MOID) of any known potentially hazardous asteroid. [6] The Earth MOID is 0.0000475 AU (7,110 km; 4,420 mi). [6] Asteroids with a smaller Earth MOID are less than ~100 meters in diameter such as 2013 XY8 and 2010 TD54. Earth impactors 2008 TC3 and 2014 AA had small Earth MOID values as they were on their impact approach when discovered.
Close-approaches to Earth[7]
DateDistance from Earth
2014-07-010.0966 AU (14,450,000 km; 8,980,000 mi) (37.6 LD)
2041-07-010.0992 AU (14,840,000 km; 9,220,000 mi) (38.6 LD)
2067-01-310.0874 AU (13,070,000 km; 8,120,000 mi) (34.0 LD)
2094-01-300.0747 AU (11,170,000 km; 6,940,000 mi) (29.1 LD)
2122-07-040.0743 AU (11,120,000 km; 6,910,000 mi) (28.9 LD)
2149-07-060.0518 AU (7,750,000 km; 4,820,000 mi) (20.2 LD)
2175-02-020.0802 AU (12,000,000 km; 7,460,000 mi) (31.2 LD)
Notes
1. At an apparent magnitude of 24, the asteroid was roughly 10 million times fainter than can be seen with the naked eye.
Math: $({\sqrt[{5}]{100}})^{24-6.5}=10000000$
References
1. "MPEC 2003-E34 : 2003 EE16". IAU Minor Planet Center. 9 March 2003. Retrieved 3 February 2014. (K03E16E)
2. "JPL Small-Body Database Browser: 177049 (2003 EE16)" (2013-03-12 last obs and observation arc=10.8 years). Jet Propulsion Laboratory. Retrieved 7 April 2016.
3. "Current Impact Risks (2003 EE16)". Near-Earth Object Program. NASA. 2 April 2003. Archived from the original on 2 April 2003.
4. "2003 EE16". Spaceguard Central Node. 15 July 2003. Archived from the original on 21 February 2014. Retrieved 3 February 2014.
5. "Date/Time Removed". NASA/JPL Near-Earth Object Program Office. Archived from the original on 2 June 2002. Retrieved 3 February 2014.
6. "JPL Small-Body Database Search Engine: H <= 22 (mag) and Earth MOID < 0.0027 (AU)". JPL Solar System Dynamics. Retrieved 3 February 2013.
7. "JPL Close-Approach Data: 177049 (2003 EE16)" (2013-03-12 last obs and observation arc=10.8 years). Retrieved 3 February 2014.
External links
• (177049) 2003 EE16 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• (177049) 2003 EE16 at ESA–space situational awareness
• Ephemerides · Observations · Orbit · Physical properties · Summary
• (177049) 2003 EE16 at the JPL Small-Body Database
Minor planets navigator
• (177049) 2003 EE16
Small Solar System bodies
Minor planets
• Designation
• Groups
• List
• Moon
• Meanings of names
Asteroid
• Active
• Aten asteroid
• Asteroid belt
• Family
• Jupiter trojan
• Near-Earth
• Spectral types
Distant minor planet
• Centaur
• Neptune trojan
• Damocloid
• Trans-Neptunian object
• Detached
• Kuiper belt
• Oort cloud
• Scattered disc
Comets
• Extinct
• Great
• Halley-type
• Hyperbolic
• Long-period
• Lost
• Near-parabolic
• Periodic
• Sungrazing
Other
• Cosmic dust
• Meteoroids
• Space debris
Authority control databases
• JPL SBDB
• MPC | 30 | 0 |
List of minor planets: 177001–178000
The following is a partial list of minor planets, running from minor-planet number 177001 through 178000, inclusive. The primary data for this and other partial lists is based on JPL's "Small-Body Orbital Elements"[1] and data available from the Minor Planet Center. [2] Critical list information is also provided by the MPC,[2] unless otherwise specified from Lowell Observatory. [3] A detailed description of the table's columns and additional sources are given on the main page including a complete list of every page in this series, and a statistical break-up on the dynamical classification of minor planets.
Also see the summary list of all named bodies in numerical and alphabetical order, and the corresponding naming citations for the number range of this particular list. New namings may only be added to this list after official publication, as the preannouncement of names is condemned by the Working Group for Small Bodies Nomenclature of the International Astronomical Union.
Near-Earth obj. MBA (inner) MBA (outer) Centaur
Mars-crosser MBA (middle) Jupiter trojan Trans-Neptunian obj.
Unclassified
• Index
• 100K
• 200K
• 300K
• 400K
• 500K
• 600K
• color code
• 172,000s
• 173,000s
• 174,000s
• 175,000s
• 176,000s
• 177,000s
• 178,000s
• 179,000s
• 180,000s
• 181,000s
• 182,000s
• 177,001…
• 177,101…
• 177,201…
• 177,301…
• 177,401…
• 177,501…
• 177,601…
• 177,701…
• 177,801…
• 177,901…
177001–177100
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1770012003 AH47—January 5, 2003SocorroLINEARCLO3.7 kmMPC · JPL
1770022003 AG59—January 5, 2003SocorroLINEAR · 6.2 kmMPC · JPL
1770032003 AC62—January 7, 2003SocorroLINEARH1.0 kmMPC · JPL
1770042003 AA85—January 7, 2003SocorroLINEAR · 3.2 kmMPC · JPL
1770052003 AV92—January 14, 2003SocorroLINEAR · 6.0 kmMPC · JPL
1770062003 BO—January 24, 2003PalomarNEAT · 5.9 kmMPC · JPL
1770072003 BW1—January 23, 2003Kitt PeakSpacewatch · 4.7 kmMPC · JPL
1770082003 BD7—January 25, 2003Anderson MesaLONEOS · 4.5 kmMPC · JPL
1770092003 BB8—January 26, 2003Kitt PeakSpacewatch · 3.3 kmMPC · JPL
1770102003 BX10—January 26, 2003Anderson MesaLONEOSJLI5.3 kmMPC · JPL
1770112003 BV19—January 26, 2003Anderson MesaLONEOS · 5.3 kmMPC · JPL
1770122003 BU24—January 25, 2003PalomarNEAT · 4.8 kmMPC · JPL
1770132003 BE26—January 26, 2003Anderson MesaLONEOSTEL2.1 kmMPC · JPL
1770142003 BZ29—January 27, 2003PalomarNEAT · 3.5 kmMPC · JPL
1770152003 BL36—January 26, 2003HaleakalaNEAT · 3.2 kmMPC · JPL
1770162003 BM47—January 31, 2003Kitt PeakSpacewatchAPO390 mMPC · JPL
1770172003 BX48—January 26, 2003HaleakalaNEAT · 4.5 kmMPC · JPL
1770182003 BU50—January 27, 2003SocorroLINEAR · 5.3 kmMPC · JPL
1770192003 BW57—January 27, 2003SocorroLINEAR · 3.4 kmMPC · JPL
1770202003 BW61—January 28, 2003SocorroLINEARALA6.8 kmMPC · JPL
1770212003 BT65—January 30, 2003SocorroLINEAR · 4.7 kmMPC · JPL
1770222003 BQ73—January 29, 2003PalomarNEATLAU1.4 kmMPC · JPL
1770232003 BW79—January 31, 2003SocorroLINEAREOS2.9 kmMPC · JPL
1770242003 BH80—January 31, 2003Anderson MesaLONEOSH840 mMPC · JPL
1770252003 BB82—January 30, 2003Anderson MesaLONEOS · 3.2 kmMPC · JPL
1770262003 BP82—January 31, 2003SocorroLINEAR · 4.1 kmMPC · JPL
1770272003 BR84—January 30, 2003HaleakalaNEAT · 4.3 kmMPC · JPL
1770282003 BX84—January 31, 2003SocorroLINEAR · 3.0 kmMPC · JPL
1770292003 BS90—January 31, 2003SocorroLINEAR · 4.4 kmMPC · JPL
1770302003 BT90—January 31, 2003SocorroLINEAR · 3.4 kmMPC · JPL
1770312003 BM92—January 28, 2003SocorroLINEAR · 4.6 kmMPC · JPL
1770322003 CU1—February 1, 2003SocorroLINEARNEM4.8 kmMPC · JPL
1770332003 CS3—February 1, 2003SocorroLINEAR · 5.4 kmMPC · JPL
1770342003 CA5—February 1, 2003SocorroLINEAREUN2.3 kmMPC · JPL
1770352003 CS6—February 1, 2003SocorroLINEAR · 6.8 kmMPC · JPL
1770362003 CG21—February 1, 2003Kitt PeakSpacewatch · 3.1 kmMPC · JPL
1770372003 CU21—February 3, 2003Anderson MesaLONEOS · 4.1 kmMPC · JPL
1770382003 CW25—February 4, 2003Kitt PeakSpacewatchHYG4.6 kmMPC · JPL
1770392003 DA5—February 19, 2003PalomarNEATYAK3.8 kmMPC · JPL
1770402003 DQ6—February 23, 2003Campo ImperatoreCINEOSH1.0 kmMPC · JPL
1770412003 DZ9—February 23, 2003SocorroLINEARH1.2 kmMPC · JPL
1770422003 DV11—February 25, 2003Campo ImperatoreCINEOSCRO5.8 kmMPC · JPL
1770432003 DL18—February 19, 2003PalomarNEAT · 4.2 kmMPC · JPL
1770442003 DK22—February 28, 2003HaleakalaNEAT · 3.0 kmMPC · JPL
1770452003 DP24—February 22, 2003PalomarNEATHYG4.1 kmMPC · JPL
1770462003 EK5—March 5, 2003SocorroLINEAR · 4.5 kmMPC · JPL
1770472003 ES5—March 5, 2003SocorroLINEAR · 6.6 kmMPC · JPL | 31 | 0 |
1770482003 EX7—March 6, 2003Anderson MesaLONEOS · 3.7 kmMPC · JPL
1770492003 EE16—March 8, 2003Kitt PeakSpacewatchAPO · PHA390 mMPC · JPL
1770502003 EW19—March 6, 2003Anderson MesaLONEOS · 3.8 kmMPC · JPL
1770512003 EG21—March 6, 2003Anderson MesaLONEOS · 4.7 kmMPC · JPL
1770522003 EA24—March 6, 2003SocorroLINEAR · 3.8 kmMPC · JPL
1770532003 EP26—March 6, 2003Anderson MesaLONEOS · 3.5 kmMPC · JPL
1770542003 EY35—March 7, 2003Anderson MesaLONEOSTHM3.6 kmMPC · JPL
1770552003 EV39—March 8, 2003SocorroLINEAR · 4.8 kmMPC · JPL
1770562003 EY41—March 8, 2003SocorroLINEAR · 4.0 kmMPC · JPL
1770572003 EB46—March 7, 2003SocorroLINEAR · 6.2 kmMPC · JPL
1770582003 EG52—March 11, 2003PalomarNEAT · 6.9 kmMPC · JPL
1770592003 EJ52—March 11, 2003PalomarNEAT · 3.8 kmMPC · JPL
1770602003 EG58—March 11, 2003SocorroLINEAR · 5.5 kmMPC · JPL
1770612003 EA59—March 12, 2003PalomarNEATEUP7.6 kmMPC · JPL
1770622003 FD3—March 24, 2003SocorroLINEARH840 mMPC · JPL
1770632003 FM3—March 24, 2003SocorroLINEARH1.1 kmMPC · JPL
1770642003 FQ4—March 26, 2003SocorroLINEAREUP8.5 kmMPC · JPL
177065 Samuelnoah2003 FP7SamuelnoahMarch 30, 2003WrightwoodJ. W. Young · 3.4 kmMPC · JPL
1770662003 FE8—March 30, 2003SocorroLINEAR · 7.2 kmMPC · JPL
1770672003 FG15—March 23, 2003CatalinaCSS · 4.7 kmMPC · JPL
1770682003 FC17—March 24, 2003Kitt PeakSpacewatchTHM2.9 kmMPC · JPL
1770692003 FR19—March 25, 2003PalomarNEAT · 6.5 kmMPC · JPL
1770702003 FN23—March 23, 2003Kitt PeakSpacewatch · 3.1 kmMPC · JPL
1770712003 FS29—March 25, 2003CatalinaCSS · 6.9 kmMPC · JPL
1770722003 FN32—March 23, 2003Kitt PeakSpacewatchTHM3.5 kmMPC · JPL
1770732003 FY33—March 23, 2003Kitt PeakSpacewatch · 2.6 kmMPC · JPL
1770742003 FD34—March 23, 2003Kitt PeakSpacewatch · 5.1 kmMPC · JPL
1770752003 FR36—March 23, 2003Kitt PeakSpacewatch · 3.9 kmMPC · JPL
1770762003 FV42—March 23, 2003CatalinaCSS · 3.6 kmMPC · JPL
1770772003 FL45—March 24, 2003Kitt PeakSpacewatch · 3.5 kmMPC · JPL
1770782003 FV45—March 24, 2003Kitt PeakSpacewatch · 4.3 kmMPC · JPL
1770792003 FA47—March 24, 2003Kitt PeakSpacewatch · 3.9 kmMPC · JPL
1770802003 FW49—March 24, 2003HaleakalaNEAT · 5.2 kmMPC · JPL
1770812003 FX52—March 25, 2003PalomarNEAT · 6.4 kmMPC · JPL
1770822003 FT55—March 26, 2003PalomarNEAT · 5.7 kmMPC · JPL
1770832003 FO56—March 26, 2003PalomarNEAT · 3.5 kmMPC · JPL
1770842003 FZ56—March 26, 2003PalomarNEAT · 3.6 kmMPC · JPL
1770852003 FU58—March 26, 2003PalomarNEAT · 4.3 kmMPC · JPL
1770862003 FE69—March 26, 2003PalomarNEAT · 6.0 kmMPC · JPL
1770872003 FY69—March 26, 2003Kitt PeakSpacewatchHYG4.0 kmMPC · JPL
1770882003 FN72—March 26, 2003PalomarNEAT · 4.6 kmMPC · JPL
1770892003 FB73—March 26, 2003HaleakalaNEATURS4.9 kmMPC · JPL
1770902003 FR73—March 26, 2003PalomarNEATALA6.2 kmMPC · JPL
1770912003 FX73—March 26, 2003HaleakalaNEATEOS3.6 kmMPC · JPL
1770922003 FD74—March 26, 2003HaleakalaNEATTHB5.9 kmMPC · JPL
1770932003 FT77—March 27, 2003PalomarNEAT · 5.8 kmMPC · JPL
1770942003 FA82—March 27, 2003SocorroLINEAR · 4.9 kmMPC · JPL
1770952003 FT88—March 28, 2003Kitt PeakSpacewatch · 5.6 kmMPC · JPL
1770962003 FP90—March 29, 2003Anderson MesaLONEOSEOS4.3 kmMPC · JPL
1770972003 FO92—March 29, 2003Anderson MesaLONEOS · 6.2 kmMPC · JPL
1770982003 FL94—March 29, 2003Anderson MesaLONEOSLIX6.4 kmMPC · JPL
1770992003 FW97—March 30, 2003Kitt PeakSpacewatch · 4.8 kmMPC · JPL
1771002003 FZ98—March 30, 2003SocorroLINEAR · 4.7 kmMPC · JPL
177101–177200
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1771012003 FW101—March 31, 2003SocorroLINEAR · 4.5 kmMPC · JPL
1771022003 FT102—March 31, 2003SocorroLINEAR · 5.5 kmMPC · JPL
1771032003 FT115—March 31, 2003SocorroLINEAR · 4.0 kmMPC · JPL
1771042003 FC116—March 31, 2003SocorroLINEAR · 6.4 kmMPC · JPL
1771052003 FM121—March 25, 2003Anderson MesaLONEOS · 5.1 kmMPC · JPL
1771062003 FC130—March 24, 2003Kitt PeakSpacewatch · 3.3 kmMPC · JPL
1771072003 FM130—March 24, 2003Kitt PeakSpacewatchTHM3.8 kmMPC · JPL
1771082003 FC131—March 22, 2003HaleakalaNEAT · 4.7 kmMPC · JPL | 31 | 1 |
1771092003 GZ2—April 1, 2003SocorroLINEAR · 6.1 kmMPC · JPL
1771102003 GZ5—April 1, 2003SocorroLINEAR · 6.1 kmMPC · JPL
1771112003 GN7—April 1, 2003SocorroLINEARHYG4.2 kmMPC · JPL
1771122003 GU10—April 3, 2003HaleakalaNEATTIR4.6 kmMPC · JPL
1771132003 GF14—April 1, 2003SocorroLINEARLIX7.8 kmMPC · JPL
1771142003 GL16—April 2, 2003HaleakalaNEATARM6.6 kmMPC · JPL
1771152003 GP16—April 3, 2003HaleakalaNEAT · 4.3 kmMPC · JPL
1771162003 GJ27—April 6, 2003Kitt PeakSpacewatch · 4.6 kmMPC · JPL
1771172003 GM27—April 7, 2003Kitt PeakSpacewatch · 3.5 kmMPC · JPL
1771182003 GM37—April 7, 2003SocorroLINEAREUP7.6 kmMPC · JPL
1771192003 GE47—April 7, 2003Kitt PeakSpacewatch · 3.4 kmMPC · JPL
177120 Ocampo Uría2003 GZ51Ocampo UríaApril 1, 2003Kitt PeakM. W. Buie · 3.7 kmMPC · JPL
1771212003 GW55—April 6, 2003Kitt PeakSpacewatch · 6.2 kmMPC · JPL
1771222003 HD3—April 24, 2003Anderson MesaLONEOS · 4.3 kmMPC · JPL
1771232003 HS5—April 21, 2003Kitt PeakSpacewatch · 4.6 kmMPC · JPL
1771242003 HV9—April 25, 2003Kitt PeakSpacewatch · 5.3 kmMPC · JPL
1771252003 HV10—April 24, 2003Kitt PeakSpacewatch · 3.6 kmMPC · JPL
1771262003 HE12—April 25, 2003Campo ImperatoreCINEOS · 4.9 kmMPC · JPL
1771272003 HO20—April 24, 2003Anderson MesaLONEOS · 6.1 kmMPC · JPL
1771282003 HU24—April 25, 2003Kitt PeakSpacewatchSAN2.3 kmMPC · JPL
1771292003 HS31—April 28, 2003Kitt PeakSpacewatchVER5.5 kmMPC · JPL
1771302003 HG43—April 29, 2003Anderson MesaLONEOS · 4.5 kmMPC · JPL
1771312003 HN51—April 30, 2003Kitt PeakSpacewatch · 3.5 kmMPC · JPL
1771322003 HA54—April 24, 2003Kitt PeakSpacewatch · 5.5 kmMPC · JPL
1771332003 JL3—May 2, 2003Kitt PeakSpacewatch · 3.1 kmMPC · JPL
1771342003 JB14—May 7, 2003CatalinaCSS · 5.2 kmMPC · JPL
1771352003 KQ11—May 25, 2003Kitt PeakSpacewatch · 4.6 kmMPC · JPL
1771362003 KK17—May 26, 2003HaleakalaNEAT · 4.7 kmMPC · JPL
1771372003 PB10—August 4, 2003SocorroLINEARNYS900 mMPC · JPL
1771382003 QE6—August 18, 2003Campo ImperatoreCINEOSFLO950 mMPC · JPL
1771392003 QC12—August 22, 2003SocorroLINEARMAS1.4 kmMPC · JPL
1771402003 QQ35—August 22, 2003PalomarNEAT · 1.2 kmMPC · JPL
1771412003 QC36—August 22, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1771422003 QT38—August 22, 2003PalomarNEAT · 1.1 kmMPC · JPL
1771432003 QV54—August 23, 2003SocorroLINEARNYS940 mMPC · JPL
1771442003 QO61—August 23, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1771452003 QZ75—August 24, 2003SocorroLINEARERI3.0 kmMPC · JPL
1771462003 QO77—August 24, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1771472003 QM79—August 25, 2003SocorroLINEARFLO1.00 kmMPC · JPL
177148 Pätzold2003 QJ85PätzoldAugust 24, 2003Cerro TololoM. W. Buie · 1.1 kmMPC · JPL
1771492003 QR95—August 30, 2003HaleakalaNEAT · 1.3 kmMPC · JPL
1771502003 RR—September 2, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1771512003 RU8—September 2, 2003SocorroLINEAR · 1.8 kmMPC · JPL
1771522003 RJ19—September 15, 2003Anderson MesaLONEOSNYS880 mMPC · JPL
1771532003 SW11—September 16, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1771542003 SH16—September 17, 2003Goodricke-PigottR. A. Tucker · 1.3 kmMPC · JPL
1771552003 SE23—September 16, 2003Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1771562003 SL31—September 18, 2003Kitt PeakSpacewatch · 810 mMPC · JPL
177157 Skoffelza2003 SF33SkoffelzaSeptember 18, 2003PiszkéstetőK. Sárneczky, B. SipőczNYS860 mMPC · JPL
1771582003 SN39—September 16, 2003PalomarNEATFLO940 mMPC · JPL
1771592003 SD47—September 16, 2003Anderson MesaLONEOS · 1.3 kmMPC · JPL
1771602003 SU83—September 18, 2003PalomarNEAT · 930 mMPC · JPL
1771612003 SG84—September 20, 2003HaleakalaNEAT · 950 mMPC · JPL
1771622003 SC97—September 19, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1771632003 SN110—September 20, 2003PalomarNEAT · 2.1 kmMPC · JPL
1771642003 ST125—September 19, 2003SocorroLINEARFLO980 mMPC · JPL
1771652003 SD128—September 20, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1771662003 SJ128—September 20, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1771672003 SL131—September 20, 2003SocorroLINEAR · 1.5 kmMPC · JPL
1771682003 SX138—September 20, 2003PalomarNEATV1.4 kmMPC · JPL
1771692003 SC144—September 21, 2003HaleakalaNEAT · 1.00 kmMPC · JPL | 31 | 2 |
1771702003 SL145—September 20, 2003PalomarNEATV1.1 kmMPC · JPL
1771712003 SE146—September 20, 2003HaleakalaNEAT · 1.2 kmMPC · JPL
1771722003 SK147—September 20, 2003PalomarNEATEUN1.9 kmMPC · JPL
1771732003 SP164—September 20, 2003Anderson MesaLONEOS · 1.2 kmMPC · JPL
1771742003 SM169—September 23, 2003HaleakalaNEAT · 1.3 kmMPC · JPL
1771752003 SM170—September 21, 2003UccleT. Pauwels · 1.4 kmMPC · JPL
1771762003 SY174—September 18, 2003Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1771772003 SG204—September 22, 2003SocorroLINEAR · 1.8 kmMPC · JPL
1771782003 SD218—September 27, 2003Kitt PeakSpacewatch · 1.0 kmMPC · JPL
1771792003 SF224—September 25, 2003Bergisch GladbachW. Bickel · 1.2 kmMPC · JPL
1771802003 SQ245—September 26, 2003SocorroLINEAR · 890 mMPC · JPL
1771812003 SE248—September 26, 2003SocorroLINEAR · 920 mMPC · JPL
1771822003 SU249—September 26, 2003SocorroLINEARNYS3.2 kmMPC · JPL
1771832003 ST263—September 28, 2003SocorroLINEAR · 1.7 kmMPC · JPL
1771842003 SU290—September 28, 2003Kitt PeakSpacewatch · 1.00 kmMPC · JPL
1771852003 TT8—October 3, 2003Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1771862003 TZ16—October 14, 2003Anderson MesaLONEOS · 860 mMPC · JPL
1771872003 TQ18—October 15, 2003Anderson MesaLONEOSV950 mMPC · JPL
1771882003 UR1—October 16, 2003Kitt PeakSpacewatch · 1.00 kmMPC · JPL
1771892003 UW4—October 17, 2003SocorroLINEARPHO1.8 kmMPC · JPL
1771902003 UA8—October 19, 2003Kitt PeakSpacewatch · 690 mMPC · JPL
1771912003 UD10—October 20, 2003Emerald LaneL. Ball · 1.2 kmMPC · JPL
1771922003 UC15—October 16, 2003Kitt PeakSpacewatch · 1.6 kmMPC · JPL
1771932003 UO15—October 16, 2003Anderson MesaLONEOS · 1.2 kmMPC · JPL
1771942003 UZ16—October 17, 2003Črni VrhČrni Vrh · 1.6 kmMPC · JPL
1771952003 UL29—October 23, 2003KvistabergUDAS · 1.4 kmMPC · JPL
1771962003 UC38—October 17, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1771972003 UV38—October 16, 2003UccleT. PauwelsNYS980 mMPC · JPL
1771982003 UB49—October 16, 2003Anderson MesaLONEOSNYS · 1.8 kmMPC · JPL
1771992003 UD54—October 18, 2003PalomarNEATV900 mMPC · JPL
1772002003 UL86—October 18, 2003PalomarNEAT · 1.4 kmMPC · JPL
177201–177300
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1772012003 UZ86—October 18, 2003PalomarNEAT · 1.2 kmMPC · JPL
1772022003 UJ91—October 20, 2003SocorroLINEAR · 1.2 kmMPC · JPL
1772032003 UF92—October 20, 2003PalomarNEATFLO1.2 kmMPC · JPL
1772042003 UP96—October 18, 2003PalomarNEATFLO1.0 kmMPC · JPL
1772052003 UU98—October 19, 2003Kitt PeakSpacewatchNYS2.7 kmMPC · JPL
1772062003 US103—October 20, 2003Kitt PeakSpacewatchNYS1.1 kmMPC · JPL
1772072003 UQ105—October 18, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1772082003 UK109—October 19, 2003Kitt PeakSpacewatchV850 mMPC · JPL
1772092003 UD117—October 21, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772102003 UE134—October 20, 2003PalomarNEAT · 1.2 kmMPC · JPL
1772112003 UZ140—October 17, 2003Campo ImperatoreCINEOSFLO1.5 kmMPC · JPL
1772122003 UN145—October 18, 2003Anderson MesaLONEOS · 3.4 kmMPC · JPL
1772132003 UT147—October 18, 2003Kitt PeakSpacewatchFLO1.1 kmMPC · JPL
1772142003 UX154—October 20, 2003Kitt PeakSpacewatch · 1.0 kmMPC · JPL
1772152003 UO159—October 20, 2003Kitt PeakSpacewatchNYS860 mMPC · JPL
1772162003 UX164—October 21, 2003PalomarNEAT · 1.1 kmMPC · JPL
1772172003 UA173—October 20, 2003PalomarNEAT · 990 mMPC · JPL
1772182003 UL174—October 21, 2003PalomarNEAT · 960 mMPC · JPL
1772192003 UO175—October 21, 2003Anderson MesaLONEOSV1.1 kmMPC · JPL
1772202003 UN188—October 22, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772212003 UW196—October 21, 2003Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1772222003 UJ208—October 22, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1772232003 UT208—October 22, 2003Kitt PeakSpacewatch · 910 mMPC · JPL
1772242003 UL218—October 21, 2003SocorroLINEARNYS910 mMPC · JPL
1772252003 UN218—October 21, 2003SocorroLINEARNYS · 3.5 kmMPC · JPL
1772262003 UE224—October 22, 2003SocorroLINEAR · 1.0 kmMPC · JPL
1772272003 UV232—October 24, 2003SocorroLINEAR · 1.0 kmMPC · JPL
1772282003 UB234—October 24, 2003SocorroLINEARV1.0 kmMPC · JPL
1772292003 UL236—October 22, 2003HaleakalaNEAT · 1.0 kmMPC · JPL
1772302003 UQ243—October 24, 2003SocorroLINEAR · 1.3 kmMPC · JPL | 31 | 3 |
1772312003 UE246—October 24, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1772322003 UY250—October 25, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1772332003 UC252—October 26, 2003CatalinaCSS · 1.0 kmMPC · JPL
1772342003 UU252—October 26, 2003Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1772352003 UK259—October 25, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1772362003 UV265—October 27, 2003HaleakalaNEAT · 1.3 kmMPC · JPL
1772372003 UH266—October 28, 2003SocorroLINEARNYS1.0 kmMPC · JPL
1772382003 UK267—October 28, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772392003 UK269—October 29, 2003SocorroLINEARV980 mMPC · JPL
1772402003 UP269—October 29, 2003SocorroLINEAR · 1.1 kmMPC · JPL
1772412003 UF276—October 29, 2003CatalinaCSS · 1.4 kmMPC · JPL
1772422003 UR276—October 30, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772432003 UH281—October 28, 2003SocorroLINEARMAS780 mMPC · JPL
1772442003 VA1—November 5, 2003SocorroLINEAR · 1.9 kmMPC · JPL
1772452003 WB—November 17, 2003WrightwoodJ. W. YoungEUN2.1 kmMPC · JPL
1772462003 WZ6—November 18, 2003PalomarNEATFLO1.0 kmMPC · JPL
1772472003 WY8—November 16, 2003Kitt PeakSpacewatchFLO820 mMPC · JPL
1772482003 WC10—November 18, 2003Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1772492003 WL11—November 18, 2003PalomarNEATV930 mMPC · JPL
1772502003 WP11—November 18, 2003PalomarNEAT · 1.3 kmMPC · JPL
1772512003 WD12—November 18, 2003PalomarNEAT · 1.3 kmMPC · JPL
1772522003 WX14—November 16, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1772532003 WL18—November 19, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772542003 WM18—November 19, 2003SocorroLINEARV1.1 kmMPC · JPL
1772552003 WC25—November 20, 2003SocorroLINEARAMO +1km1.7 kmMPC · JPL
1772562003 WA30—November 18, 2003Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1772572003 WP32—November 18, 2003Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1772582003 WX39—November 19, 2003Kitt PeakSpacewatchERI2.5 kmMPC · JPL
1772592003 WT55—November 20, 2003SocorroLINEARNYS2.9 kmMPC · JPL
1772602003 WM56—November 20, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772612003 WF57—November 18, 2003PalomarNEAT · 1.4 kmMPC · JPL
1772622003 WA58—November 18, 2003Kitt PeakSpacewatchERI2.5 kmMPC · JPL
1772632003 WY59—November 18, 2003PalomarNEAT · 1.3 kmMPC · JPL
1772642003 WQ64—November 19, 2003Kitt PeakSpacewatchNYS1.0 kmMPC · JPL
1772652003 WX75—November 19, 2003SocorroLINEARV810 mMPC · JPL
1772662003 WK88—November 24, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1772672003 WM92—November 18, 2003PalomarNEATV1.0 kmMPC · JPL
1772682003 WF95—November 19, 2003Anderson MesaLONEOSV970 mMPC · JPL
1772692003 WV101—November 21, 2003SocorroLINEAR · 890 mMPC · JPL
1772702003 WB114—November 20, 2003SocorroLINEAR · 1.8 kmMPC · JPL
1772712003 WJ117—November 20, 2003SocorroLINEARV1.0 kmMPC · JPL
1772722003 WO122—November 20, 2003SocorroLINEARFLO930 mMPC · JPL
1772732003 WW126—November 20, 2003SocorroLINEAR · 1.2 kmMPC · JPL
1772742003 WM129—November 21, 2003SocorroLINEARFLO910 mMPC · JPL
1772752003 WH132—November 19, 2003Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1772762003 WB135—November 21, 2003SocorroLINEAR · 2.1 kmMPC · JPL
1772772003 WN135—November 21, 2003SocorroLINEAREUN1.9 kmMPC · JPL
1772782003 WR138—November 21, 2003SocorroLINEARNYS1.2 kmMPC · JPL
1772792003 WD142—November 21, 2003SocorroLINEAR · 1.5 kmMPC · JPL
1772802003 WY142—November 23, 2003SocorroLINEAR · 2.7 kmMPC · JPL
1772812003 WE149—November 24, 2003SocorroLINEARNYS1.8 kmMPC · JPL
1772822003 WQ151—November 28, 2003SandlotG. HugNYS1.1 kmMPC · JPL
1772832003 WG152—November 28, 2003Kitt PeakSpacewatchFLO750 mMPC · JPL
1772842003 WS152—November 26, 2003SocorroLINEARPHO2.0 kmMPC · JPL
1772852003 WE155—November 26, 2003Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1772862003 WX162—November 30, 2003Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1772872003 WF166—November 20, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1772882003 XF—December 3, 2003SocorroLINEAR · 2.0 kmMPC · JPL
1772892003 XA1—December 1, 2003Kitt PeakSpacewatchV930 mMPC · JPL
1772902003 XD1—December 1, 2003Kitt PeakSpacewatchV970 mMPC · JPL
1772912003 XR6—December 3, 2003SocorroLINEARNYS1.1 kmMPC · JPL
1772922003 XA12—December 14, 2003SocorroLINEAR · 2.5 kmMPC · JPL
1772932003 XM12—December 14, 2003PalomarNEAT · 2.8 kmMPC · JPL
1772942003 XO17—December 15, 2003Kitt PeakSpacewatch · 3.5 kmMPC · JPL | 31 | 4 |
1772952003 XX17—December 14, 2003Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1772962003 XK19—December 15, 2003SocorroLINEAR · 3.8 kmMPC · JPL
1772972003 XD28—December 1, 2003Kitt PeakSpacewatchNYS810 mMPC · JPL
1772982003 XP30—December 1, 2003Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1772992003 YB1—December 17, 2003SocorroLINEAR · 1.6 kmMPC · JPL
1773002003 YH4—December 16, 2003CatalinaCSS · 1.3 kmMPC · JPL
177301–177400
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1773012003 YA5—December 16, 2003CatalinaCSSFLO800 mMPC · JPL
1773022003 YB7—December 17, 2003SocorroLINEARV1.2 kmMPC · JPL
1773032003 YG7—December 17, 2003Kitt PeakSpacewatchNYS1.1 kmMPC · JPL
1773042003 YZ12—December 17, 2003Anderson MesaLONEOSNYS1.00 kmMPC · JPL
1773052003 YW14—December 17, 2003SocorroLINEAR · 1.2 kmMPC · JPL
1773062003 YE15—December 17, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1773072003 YC18—December 16, 2003Anderson MesaLONEOS · 1.9 kmMPC · JPL
1773082003 YR19—December 17, 2003Kitt PeakSpacewatch · 2.4 kmMPC · JPL
1773092003 YX19—December 17, 2003Kitt PeakSpacewatch · 1.0 kmMPC · JPL
1773102003 YD22—December 18, 2003SocorroLINEARV1.0 kmMPC · JPL
1773112003 YS29—December 17, 2003Kitt PeakSpacewatchNYS1.3 kmMPC · JPL
1773122003 YC32—December 18, 2003SocorroLINEARV1.2 kmMPC · JPL
1773132003 YT32—December 16, 2003Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1773142003 YE33—December 16, 2003CatalinaCSS · 1.4 kmMPC · JPL
1773152003 YO33—December 17, 2003CatalinaCSS · 1.1 kmMPC · JPL
1773162003 YY34—December 18, 2003SocorroLINEARV1.1 kmMPC · JPL
1773172003 YW35—December 19, 2003SocorroLINEAR · 4.2 kmMPC · JPL
1773182003 YR36—December 17, 2003PalomarNEAT · 2.2 kmMPC · JPL
1773192003 YS41—December 19, 2003Kitt PeakSpacewatchMAS1.1 kmMPC · JPL
1773202003 YG42—December 19, 2003Kitt PeakSpacewatchHEN1.1 kmMPC · JPL
1773212003 YT43—December 19, 2003SocorroLINEAR · 1.6 kmMPC · JPL
1773222003 YX43—December 19, 2003Kitt PeakSpacewatch · 1.6 kmMPC · JPL
1773232003 YO48—December 18, 2003SocorroLINEAR · 2.0 kmMPC · JPL
1773242003 YR48—December 18, 2003SocorroLINEARMAR3.1 kmMPC · JPL
1773252003 YJ49—December 18, 2003SocorroLINEAR · 1.2 kmMPC · JPL
1773262003 YN57—December 19, 2003SocorroLINEAREUN2.2 kmMPC · JPL
1773272003 YX57—December 19, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1773282003 YC61—December 19, 2003SocorroLINEARNYS900 mMPC · JPL
1773292003 YP62—December 19, 2003SocorroLINEAR · 1.7 kmMPC · JPL
1773302003 YR66—December 20, 2003SocorroLINEAR · 4.3 kmMPC · JPL
1773312003 YJ70—December 21, 2003HaleakalaNEATHNS2.0 kmMPC · JPL
1773322003 YL70—December 21, 2003CatalinaCSS · 2.4 kmMPC · JPL
1773332003 YH77—December 18, 2003SocorroLINEARMAS860 mMPC · JPL
1773342003 YW78—December 18, 2003SocorroLINEAR · 2.7 kmMPC · JPL
1773352003 YZ87—December 19, 2003SocorroLINEAR · 1.5 kmMPC · JPL
1773362003 YS99—December 19, 2003SocorroLINEARFLO1.1 kmMPC · JPL
1773372003 YG100—December 19, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1773382003 YN106—December 22, 2003Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1773392003 YK114—December 25, 2003HaleakalaNEAT · 3.9 kmMPC · JPL
1773402003 YO120—December 27, 2003SocorroLINEAR · 1.5 kmMPC · JPL
1773412003 YF123—December 27, 2003SocorroLINEARRAF1.6 kmMPC · JPL
1773422003 YX127—December 27, 2003SocorroLINEAR · 3.5 kmMPC · JPL
1773432003 YA128—December 27, 2003SocorroLINEARV1.1 kmMPC · JPL
1773442003 YN128—December 27, 2003SocorroLINEAR · 1.8 kmMPC · JPL
1773452003 YO128—December 27, 2003SocorroLINEAR · 1.5 kmMPC · JPL
1773462003 YG130—December 27, 2003SocorroLINEARGEF2.4 kmMPC · JPL
1773472003 YP133—December 28, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1773482003 YP137—December 27, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1773492003 YH138—December 27, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1773502003 YA145—December 28, 2003SocorroLINEAR · 4.4 kmMPC · JPL
1773512003 YV149—December 29, 2003SocorroLINEAR · 1.3 kmMPC · JPL
1773522003 YL157—December 16, 2003Kitt PeakSpacewatchV1.1 kmMPC · JPL
1773532003 YJ161—December 17, 2003SocorroLINEAR · 1.4 kmMPC · JPL
1773542003 YH180—December 18, 2003Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1773552004 AP1—January 12, 2004PalomarNEAT · 1.4 kmMPC · JPL | 31 | 5 |
1773562004 AV3—January 13, 2004Anderson MesaLONEOSV1.3 kmMPC · JPL
1773572004 AM5—January 13, 2004Anderson MesaLONEOS · 1.6 kmMPC · JPL
1773582004 AA10—January 15, 2004Kitt PeakSpacewatch · 1.0 kmMPC · JPL
1773592004 BT3—January 16, 2004PalomarNEATMAS1.1 kmMPC · JPL
1773602004 BU4—January 16, 2004PalomarNEATNYS1.3 kmMPC · JPL
1773612004 BW5—January 16, 2004Kitt PeakSpacewatchNYS1.0 kmMPC · JPL
1773622004 BZ5—January 16, 2004Kitt PeakSpacewatchMAS1.1 kmMPC · JPL
1773632004 BS11—January 16, 2004PalomarNEAT · 1.4 kmMPC · JPL
1773642004 BF15—January 16, 2004Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1773652004 BM15—January 16, 2004Kitt PeakSpacewatch · 1.9 kmMPC · JPL
1773662004 BM19—January 17, 2004PalomarNEAT · 1.3 kmMPC · JPL
1773672004 BD20—January 18, 2004PalomarNEAT · 1.8 kmMPC · JPL
1773682004 BH24—January 19, 2004Anderson MesaLONEOS · 1.8 kmMPC · JPL
1773692004 BQ28—January 18, 2004PalomarNEAT · 2.0 kmMPC · JPL
1773702004 BT31—January 19, 2004Anderson MesaLONEOS · 2.3 kmMPC · JPL
1773712004 BY33—January 19, 2004Kitt PeakSpacewatch · 2.7 kmMPC · JPL
1773722004 BE36—January 19, 2004Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1773732004 BB37—January 19, 2004Kitt PeakSpacewatchNYS1.1 kmMPC · JPL
1773742004 BT39—January 21, 2004SocorroLINEARJUN1.3 kmMPC · JPL
1773752004 BH51—January 21, 2004SocorroLINEAR · 2.9 kmMPC · JPL
1773762004 BW54—January 22, 2004SocorroLINEARNYS1.2 kmMPC · JPL
1773772004 BR57—January 23, 2004SocorroLINEAR · 1.8 kmMPC · JPL
1773782004 BX57—January 23, 2004Anderson MesaLONEOS · 2.0 kmMPC · JPL
1773792004 BD58—January 23, 2004SocorroLINEAR · 1.5 kmMPC · JPL
1773802004 BE60—January 21, 2004SocorroLINEARMAS1.3 kmMPC · JPL
1773812004 BP60—January 21, 2004SocorroLINEAR · 1.9 kmMPC · JPL
1773822004 BW62—January 22, 2004SocorroLINEARNYS1.1 kmMPC · JPL
1773832004 BC63—January 22, 2004SocorroLINEAR · 1.1 kmMPC · JPL
1773842004 BS70—January 22, 2004SocorroLINEARV1.1 kmMPC · JPL
1773852004 BG72—January 23, 2004SocorroLINEAR · 1.6 kmMPC · JPL
1773862004 BY73—January 24, 2004SocorroLINEARADE4.1 kmMPC · JPL
1773872004 BA74—January 24, 2004SocorroLINEAREUT1.1 kmMPC · JPL
1773882004 BF80—January 24, 2004SocorroLINEAR · 1.3 kmMPC · JPL
1773892004 BS82—January 23, 2004SocorroLINEAR · 2.3 kmMPC · JPL
1773902004 BA83—January 28, 2004Kitt PeakSpacewatchEUN2.1 kmMPC · JPL
1773912004 BX83—January 23, 2004SocorroLINEAR · 2.9 kmMPC · JPL
1773922004 BD84—January 24, 2004SocorroLINEARNYS1.0 kmMPC · JPL
1773932004 BH88—January 23, 2004SocorroLINEARV1.0 kmMPC · JPL
1773942004 BV89—January 23, 2004SocorroLINEARADE3.1 kmMPC · JPL
1773952004 BU93—January 28, 2004SocorroLINEAR · 3.0 kmMPC · JPL
1773962004 BY93—January 28, 2004SocorroLINEAR · 3.5 kmMPC · JPL
1773972004 BA94—January 28, 2004HaleakalaNEAT · 1.7 kmMPC · JPL
1773982004 BE104—January 23, 2004SocorroLINEAR · 1.9 kmMPC · JPL
1773992004 BR104—January 23, 2004SocorroLINEAR · 4.1 kmMPC · JPL
1774002004 BB107—January 28, 2004Kitt PeakSpacewatch · 1.5 kmMPC · JPL
177401–177500
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1774012004 BK107—January 28, 2004CatalinaCSS · 1.5 kmMPC · JPL
1774022004 BV107—January 28, 2004CatalinaCSSBRU3.4 kmMPC · JPL
1774032004 BA110—January 28, 2004CatalinaCSSHNS3.4 kmMPC · JPL
1774042004 BC110—January 28, 2004CatalinaCSS · 1.9 kmMPC · JPL
1774052004 BK119—January 30, 2004SocorroLINEAR · 1.8 kmMPC · JPL
1774062004 BU145—January 21, 2004SocorroLINEARV1.1 kmMPC · JPL
1774072004 BT146—January 22, 2004SocorroLINEARMAS1.1 kmMPC · JPL
1774082004 BC147—January 22, 2004SocorroLINEAR · 1.5 kmMPC · JPL
1774092004 BS149—January 16, 2004Kitt PeakSpacewatchNYS1.2 kmMPC · JPL
1774102004 BQ152—January 26, 2004Anderson MesaLONEOS · 1.5 kmMPC · JPL
1774112004 BE162—January 16, 2004PalomarNEAT · 1.5 kmMPC · JPL
1774122004 CK—February 2, 2004SocorroLINEARJUN1.4 kmMPC · JPL
1774132004 CF2—February 12, 2004Desert EagleW. K. Y. YeungEUN1.6 kmMPC · JPL
1774142004 CL2—February 11, 2004PalomarNEATHNS1.9 kmMPC · JPL
177415 Queloz2004 CK3QuelozFebruary 9, 2004VicquesM. Ory · 2.4 kmMPC · JPL
1774162004 CB5—February 10, 2004NogalesTenagra II Obs.MAS1.0 kmMPC · JPL | 31 | 6 |
1774172004 CD5—February 10, 2004PalomarNEAT · 3.1 kmMPC · JPL
1774182004 CT10—February 11, 2004PalomarNEATNYS1.0 kmMPC · JPL
1774192004 CG12—February 11, 2004CatalinaCSSMAS1.5 kmMPC · JPL
1774202004 CX12—February 11, 2004PalomarNEAT · 1.8 kmMPC · JPL
1774212004 CC13—February 11, 2004PalomarNEATMAR2.1 kmMPC · JPL
1774222004 CC18—February 10, 2004PalomarNEAT · 2.7 kmMPC · JPL
1774232004 CL27—February 11, 2004PalomarNEATNYS1.6 kmMPC · JPL
1774242004 CC28—February 12, 2004Kitt PeakSpacewatchMAS1.2 kmMPC · JPL
1774252004 CA37—February 12, 2004PalomarNEAT · 1.7 kmMPC · JPL
1774262004 CZ49—February 11, 2004PalomarNEAT · 2.0 kmMPC · JPL
1774272004 CX50—February 11, 2004Anderson MesaLONEOSGEF2.1 kmMPC · JPL
1774282004 CY54—February 11, 2004PalomarNEAT · 1.5 kmMPC · JPL
1774292004 CQ63—February 12, 2004PalomarNEAT · 3.5 kmMPC · JPL
1774302004 CG64—February 13, 2004Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1774312004 CH68—February 11, 2004Anderson MesaLONEOS · 1.1 kmMPC · JPL
1774322004 CO71—February 13, 2004PalomarNEAT · 1.8 kmMPC · JPL
1774332004 CN72—February 13, 2004Kitt PeakSpacewatch · 1.9 kmMPC · JPL
1774342004 CP78—February 11, 2004PalomarNEAT · 2.4 kmMPC · JPL
1774352004 CL79—February 11, 2004Kitt PeakSpacewatchNYS1.3 kmMPC · JPL
1774362004 CA80—February 11, 2004PalomarNEATMAS1.1 kmMPC · JPL
1774372004 CQ92—February 14, 2004HaleakalaNEATHNS1.9 kmMPC · JPL
1774382004 CK94—February 11, 2004PalomarNEATMAS1.4 kmMPC · JPL
1774392004 CJ95—February 13, 2004PalomarNEAT · 2.6 kmMPC · JPL
1774402004 CL95—February 13, 2004PalomarNEATADE3.4 kmMPC · JPL
1774412004 CD96—February 14, 2004Kitt PeakSpacewatch · 2.0 kmMPC · JPL
1774422004 CW98—February 14, 2004CatalinaCSS · 1.4 kmMPC · JPL
1774432004 CA105—February 13, 2004PalomarNEAT · 2.7 kmMPC · JPL
1774442004 CD105—February 13, 2004PalomarNEAT · 5.7 kmMPC · JPL
1774452004 CZ106—February 14, 2004PalomarNEATMAR1.8 kmMPC · JPL
1774462004 CW107—February 14, 2004Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1774472004 CZ115—February 11, 2004Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1774482004 DA8—February 17, 2004Kitt PeakSpacewatch · 2.0 kmMPC · JPL
1774492004 DY10—February 16, 2004Kitt PeakSpacewatch · 4.5 kmMPC · JPL
1774502004 DH11—February 16, 2004Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1774512004 DQ12—February 16, 2004CatalinaCSS · 1.6 kmMPC · JPL
1774522004 DC16—February 17, 2004Kitt PeakSpacewatch · 4.6 kmMPC · JPL
1774532004 DS17—February 18, 2004Kitt PeakSpacewatch · 2.2 kmMPC · JPL
1774542004 DC19—February 16, 2004CatalinaCSSV1.2 kmMPC · JPL
1774552004 DM19—February 17, 2004SocorroLINEAR · 2.5 kmMPC · JPL
1774562004 DE21—February 17, 2004CatalinaCSS · 4.9 kmMPC · JPL
1774572004 DH36—February 19, 2004SocorroLINEAR · 1.1 kmMPC · JPL
1774582004 DO37—February 19, 2004SocorroLINEAREUN1.6 kmMPC · JPL
1774592004 DS37—February 19, 2004SocorroLINEAR · 1.5 kmMPC · JPL
1774602004 DL41—February 18, 2004HaleakalaNEAT · 2.4 kmMPC · JPL
1774612004 DV41—February 19, 2004SocorroLINEAR · 1.4 kmMPC · JPL
1774622004 DP42—February 19, 2004SocorroLINEAR · 3.4 kmMPC · JPL
1774632004 DZ42—February 23, 2004SocorroLINEAR · 1.6 kmMPC · JPL
1774642004 DF48—February 19, 2004SocorroLINEARNYS1.0 kmMPC · JPL
1774652004 DQ50—February 23, 2004SocorroLINEAR · 1.5 kmMPC · JPL
1774662004 DQ51—February 23, 2004SocorroLINEARMIS3.2 kmMPC · JPL
1774672004 DG57—February 23, 2004SocorroLINEARMAR2.2 kmMPC · JPL
1774682004 DN60—February 26, 2004SocorroLINEAR · 1.7 kmMPC · JPL
1774692004 DR70—February 26, 2004SocorroLINEAR · 2.3 kmMPC · JPL
1774702004 DV71—February 17, 2004SocorroLINEARMAR1.6 kmMPC · JPL
1774712004 DU72—February 17, 2004PalomarNEATV1.3 kmMPC · JPL
1774722004 DX75—February 17, 2004SocorroLINEARNYS1.1 kmMPC · JPL
1774732004 DF76—February 17, 2004Kitt PeakSpacewatchHEN1.5 kmMPC · JPL
1774742004 EJ4—March 11, 2004PalomarNEATADE4.1 kmMPC · JPL
1774752004 EZ4—March 11, 2004PalomarNEAT · 1.3 kmMPC · JPL
1774762004 ET8—March 13, 2004PalomarNEATMIS3.2 kmMPC · JPL
1774772004 EA10—March 12, 2004PalomarNEAT · 3.7 kmMPC · JPL
1774782004 EC11—March 15, 2004Desert EagleW. K. Y. Yeung · 1.6 kmMPC · JPL
1774792004 EA14—March 11, 2004PalomarNEAT · 2.3 kmMPC · JPL | 31 | 7 |
1774802004 EX14—March 11, 2004PalomarNEAT · 2.1 kmMPC · JPL
1774812004 EH16—March 12, 2004PalomarNEAT · 2.2 kmMPC · JPL
1774822004 EV16—March 12, 2004PalomarNEATINO2.0 kmMPC · JPL
1774832004 EJ18—March 12, 2004PalomarNEAT · 3.3 kmMPC · JPL
1774842004 EK19—March 14, 2004Kitt PeakSpacewatch · 1.8 kmMPC · JPL
1774852004 ET19—March 14, 2004Kitt PeakSpacewatch · 3.7 kmMPC · JPL
1774862004 EZ29—March 15, 2004Kitt PeakSpacewatch · 3.3 kmMPC · JPL
1774872004 EX31—March 14, 2004PalomarNEAT · 2.2 kmMPC · JPL
1774882004 EG32—March 15, 2004Kitt PeakSpacewatch · 2.3 kmMPC · JPL
1774892004 EY32—March 15, 2004PalomarNEAT · 3.4 kmMPC · JPL
1774902004 EW34—March 12, 2004PalomarNEAT · 1.2 kmMPC · JPL
1774912004 ED37—March 13, 2004PalomarNEAT · 5.1 kmMPC · JPL
1774922004 EB38—March 14, 2004PalomarNEAT · 2.7 kmMPC · JPL
1774932004 EB40—March 15, 2004SocorroLINEAR · 5.3 kmMPC · JPL
1774942004 EE41—March 15, 2004CatalinaCSS · 3.7 kmMPC · JPL
1774952004 EG41—March 15, 2004SocorroLINEAR · 1.4 kmMPC · JPL
1774962004 EN47—March 15, 2004CatalinaCSS · 2.4 kmMPC · JPL
1774972004 EV47—March 15, 2004CatalinaCSS · 2.0 kmMPC · JPL
1774982004 EC48—March 15, 2004CatalinaCSS · 2.0 kmMPC · JPL
1774992004 EF50—March 12, 2004PalomarNEAT · 990 mMPC · JPL
1775002004 EV52—March 15, 2004CatalinaCSSWAT3.8 kmMPC · JPL
177501–177600
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1775012004 EW52—March 15, 2004SocorroLINEAR · 2.9 kmMPC · JPL
1775022004 EZ52—March 15, 2004SocorroLINEAR · 2.6 kmMPC · JPL
1775032004 EE53—March 15, 2004SocorroLINEARGEF2.2 kmMPC · JPL
1775042004 EN56—March 14, 2004PalomarNEAT · 2.1 kmMPC · JPL
1775052004 EP56—March 14, 2004PalomarNEATRAF1.6 kmMPC · JPL
1775062004 ED58—March 15, 2004CatalinaCSS · 1.8 kmMPC · JPL
1775072004 EO58—March 15, 2004SocorroLINEAREUN1.4 kmMPC · JPL
1775082004 EZ58—March 15, 2004PalomarNEAT · 4.1 kmMPC · JPL
1775092004 EM59—March 15, 2004PalomarNEAT · 2.8 kmMPC · JPL
1775102004 EP64—March 14, 2004SocorroLINEARINO1.9 kmMPC · JPL
1775112004 EW64—March 14, 2004SocorroLINEARKRM4.5 kmMPC · JPL
1775122004 EA65—March 14, 2004SocorroLINEAR · 3.8 kmMPC · JPL
1775132004 EH65—March 14, 2004SocorroLINEAREUN1.9 kmMPC · JPL
1775142004 EG67—March 15, 2004Kitt PeakSpacewatch · 1.9 kmMPC · JPL
1775152004 ER67—March 15, 2004Kitt PeakSpacewatch · 3.2 kmMPC · JPL
1775162004 EB71—March 15, 2004CatalinaCSS · 1.1 kmMPC · JPL
1775172004 ED74—March 12, 2004PalomarNEAT · 1.8 kmMPC · JPL
1775182004 EK77—March 15, 2004SocorroLINEAR · 3.9 kmMPC · JPL
1775192004 EW79—March 12, 2004PalomarNEATGER2.3 kmMPC · JPL
1775202004 ET81—March 15, 2004SocorroLINEAR · 2.6 kmMPC · JPL
1775212004 EK83—March 14, 2004Kitt PeakSpacewatchCHA3.2 kmMPC · JPL
1775222004 EP86—March 15, 2004Kitt PeakSpacewatchAER1.9 kmMPC · JPL
1775232004 EO94—March 15, 2004CatalinaCSS · 3.9 kmMPC · JPL
1775242004 EA100—March 15, 2004Kitt PeakSpacewatch · 2.2 kmMPC · JPL
1775252004 FS11—March 16, 2004CatalinaCSS · 4.9 kmMPC · JPL
1775262004 FC16—March 23, 2004Goodricke-PigottR. A. Tucker · 3.9 kmMPC · JPL
1775272004 FK19—March 16, 2004CatalinaCSS · 3.0 kmMPC · JPL
1775282004 FV19—March 16, 2004SocorroLINEARTIN4.5 kmMPC · JPL
1775292004 FK20—March 16, 2004SocorroLINEAR · 2.3 kmMPC · JPL
1775302004 FP21—March 16, 2004Kitt PeakSpacewatchAGN1.6 kmMPC · JPL
1775312004 FR21—March 16, 2004Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1775322004 FX23—March 17, 2004Kitt PeakSpacewatch · 3.0 kmMPC · JPL
1775332004 FX24—March 17, 2004SocorroLINEARMAR1.8 kmMPC · JPL
1775342004 FA28—March 17, 2004Kitt PeakSpacewatchWIT1.5 kmMPC · JPL
1775352004 FV29—March 27, 2004Bergisch GladbachW. Bickel · 4.6 kmMPC · JPL
1775362004 FT34—March 16, 2004SocorroLINEARRAF1.6 kmMPC · JPL
1775372004 FO37—March 17, 2004Kitt PeakSpacewatch · 4.4 kmMPC · JPL
1775382004 FT48—March 18, 2004SocorroLINEARMAR2.0 kmMPC · JPL
1775392004 FZ53—March 18, 2004SocorroLINEAR · 3.3 kmMPC · JPL
1775402004 FU55—March 20, 2004SocorroLINEARNEM5.3 kmMPC · JPL | 31 | 8 |
1775412004 FA56—March 20, 2004SocorroLINEAR · 3.1 kmMPC · JPL
1775422004 FC59—March 18, 2004Kitt PeakSpacewatch · 2.7 kmMPC · JPL
1775432004 FM63—March 19, 2004SocorroLINEAR · 3.7 kmMPC · JPL
1775442004 FS63—March 19, 2004SocorroLINEAR · 1.4 kmMPC · JPL
1775452004 FZ63—March 19, 2004SocorroLINEARGEF2.3 kmMPC · JPL
1775462004 FB66—March 19, 2004SocorroLINEAR · 2.5 kmMPC · JPL
1775472004 FJ67—March 20, 2004SocorroLINEAR · 4.0 kmMPC · JPL
1775482004 FW67—March 20, 2004SocorroLINEAR · 2.3 kmMPC · JPL
1775492004 FB68—March 20, 2004SocorroLINEAR · 2.8 kmMPC · JPL
1775502004 FZ68—March 16, 2004Kitt PeakSpacewatch · 2.2 kmMPC · JPL
1775512004 FO81—March 16, 2004SocorroLINEAR · 3.7 kmMPC · JPL
1775522004 FR83—March 18, 2004PalomarNEAT · 3.8 kmMPC · JPL
1775532004 FR84—March 18, 2004SocorroLINEAR · 1.9 kmMPC · JPL
1775542004 FB86—March 19, 2004PalomarNEATMAR1.6 kmMPC · JPL
1775552004 FB91—March 21, 2004Kitt PeakSpacewatch · 3.9 kmMPC · JPL
1775562004 FW91—March 22, 2004SocorroLINEAR · 3.3 kmMPC · JPL
1775572004 FV96—March 23, 2004SocorroLINEAR · 2.3 kmMPC · JPL
1775582004 FQ98—March 19, 2004SocorroLINEAR · 3.5 kmMPC · JPL
1775592004 FR98—March 19, 2004SocorroLINEARNEM3.6 kmMPC · JPL
1775602004 FZ101—March 19, 2004SocorroLINEAR · 2.9 kmMPC · JPL
1775612004 FN105—March 24, 2004Siding SpringSSSHNS2.1 kmMPC · JPL
1775622004 FS105—March 25, 2004SocorroLINEAR · 2.7 kmMPC · JPL
1775632004 FD107—March 20, 2004SocorroLINEAR · 3.5 kmMPC · JPL
1775642004 FN109—March 24, 2004Anderson MesaLONEOSNEM4.0 kmMPC · JPL
1775652004 FZ115—March 23, 2004SocorroLINEAR · 3.8 kmMPC · JPL
1775662004 FM116—March 23, 2004SocorroLINEAR · 1.7 kmMPC · JPL
1775672004 FC119—March 23, 2004Kitt PeakSpacewatch · 1.8 kmMPC · JPL
1775682004 FS119—March 23, 2004Kitt PeakSpacewatch · 3.7 kmMPC · JPL
1775692004 FT120—March 23, 2004SocorroLINEAR · 2.6 kmMPC · JPL
1775702004 FX120—March 23, 2004SocorroLINEAR · 2.7 kmMPC · JPL
1775712004 FY125—March 27, 2004SocorroLINEAR · 2.4 kmMPC · JPL
1775722004 FU126—March 27, 2004SocorroLINEAR · 4.3 kmMPC · JPL
1775732004 FW131—March 23, 2004Kitt PeakSpacewatchHEN1.4 kmMPC · JPL
1775742004 FM134—March 26, 2004SocorroLINEAR · 4.6 kmMPC · JPL
1775752004 FD138—March 29, 2004Kitt PeakSpacewatch · 1.6 kmMPC · JPL
1775762004 FQ138—March 17, 2004SocorroLINEAR · 2.7 kmMPC · JPL
1775772004 FW145—March 30, 2004Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1775782004 FL152—March 17, 2004Kitt PeakSpacewatchKAR1.5 kmMPC · JPL
1775792004 FW158—March 18, 2004Kitt PeakSpacewatch · 2.2 kmMPC · JPL
1775802004 GK2—April 12, 2004Siding SpringSSS · 1.9 kmMPC · JPL
1775812004 GS7—April 12, 2004Anderson MesaLONEOS · 2.0 kmMPC · JPL
1775822004 GC8—April 12, 2004Anderson MesaLONEOSNEM3.1 kmMPC · JPL
1775832004 GT9—April 10, 2004KvistabergUDASMAR1.9 kmMPC · JPL
1775842004 GJ11—April 13, 2004SocorroLINEAR · 4.1 kmMPC · JPL
1775852004 GN13—April 13, 2004PalomarNEATJUN2.2 kmMPC · JPL
1775862004 GH14—April 13, 2004CatalinaCSS · 1.8 kmMPC · JPL
1775872004 GH16—April 10, 2004PalomarNEAT · 5.5 kmMPC · JPL
1775882004 GW16—April 10, 2004CatalinaCSSEUN2.3 kmMPC · JPL
1775892004 GT21—April 11, 2004PalomarNEAT · 5.9 kmMPC · JPL
1775902004 GJ26—April 14, 2004Anderson MesaLONEOSAEO2.3 kmMPC · JPL
1775912004 GV37—April 14, 2004Anderson MesaLONEOSDOR3.7 kmMPC · JPL
1775922004 GR38—April 15, 2004CatalinaCSS · 2.6 kmMPC · JPL
1775932004 GR39—April 15, 2004Siding SpringSSS · 3.4 kmMPC · JPL
1775942004 GK41—April 12, 2004Siding SpringSSSCLO3.5 kmMPC · JPL
1775952004 GD44—April 12, 2004PalomarNEAT · 2.5 kmMPC · JPL
1775962004 GS47—April 12, 2004Kitt PeakSpacewatch · 3.9 kmMPC · JPL
1775972004 GB48—April 12, 2004Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1775982004 GJ48—April 12, 2004Kitt PeakSpacewatch · 1.6 kmMPC · JPL
1775992004 GJ57—April 14, 2004Kitt PeakSpacewatchAGN1.5 kmMPC · JPL
1776002004 GJ59—April 12, 2004PalomarNEAT · 3.1 kmMPC · JPL
177601–177700
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1776012004 GN73—April 14, 2004Bergisch GladbachW. Bickel · 1.2 kmMPC · JPL | 31 | 9 |
1776022004 GW74—April 15, 2004SocorroLINEAR · 4.0 kmMPC · JPL
1776032004 GD75—April 14, 2004Anderson MesaLONEOS · 3.6 kmMPC · JPL
1776042004 GY75—April 15, 2004Siding SpringSSS · 4.7 kmMPC · JPL
1776052004 GJ78—April 9, 2004Siding SpringSSS · 1.7 kmMPC · JPL
1776062004 GY81—April 13, 2004CatalinaCSS · 2.2 kmMPC · JPL
1776072004 HD1—April 19, 2004Siding SpringSSSBRU6.0 kmMPC · JPL
1776082004 HC5—April 16, 2004PalomarNEAT · 3.1 kmMPC · JPL
1776092004 HY6—April 16, 2004SocorroLINEAR · 2.5 kmMPC · JPL
1776102004 HE10—April 17, 2004SocorroLINEAR · 4.4 kmMPC · JPL
1776112004 HO15—April 16, 2004Kitt PeakSpacewatchAGN1.8 kmMPC · JPL
1776122004 HK24—April 16, 2004SocorroLINEAR · 4.3 kmMPC · JPL
1776132004 HK31—April 16, 2004PalomarNEAT · 4.5 kmMPC · JPL
1776142004 HK33—April 21, 2004SocorroLINEARAPO +1km · PHA1.1 kmMPC · JPL
1776152004 HB44—April 21, 2004SocorroLINEAR · 4.1 kmMPC · JPL
1776162004 HX47—April 22, 2004Siding SpringSSSGEF2.3 kmMPC · JPL
1776172004 HR48—April 22, 2004Siding SpringSSS · 4.2 kmMPC · JPL
1776182004 HA54—April 22, 2004CatalinaCSSTIN3.0 kmMPC · JPL
1776192004 HB56—April 24, 2004Siding SpringSSS · 3.6 kmMPC · JPL
1776202004 HC58—April 22, 2004Kitt PeakSpacewatchKOR1.5 kmMPC · JPL
1776212004 HN60—April 25, 2004SocorroLINEAR · 1.8 kmMPC · JPL
1776222004 HF61—April 25, 2004SocorroLINEAR · 2.6 kmMPC · JPL
1776232004 HU61—April 25, 2004SocorroLINEAR · 2.0 kmMPC · JPL
1776242004 HB73—April 28, 2004Kitt PeakSpacewatchHYG3.5 kmMPC · JPL
177625 Dembicky2004 JDDembickyMay 8, 2004WrightwoodJ. W. Young · 3.3 kmMPC · JPL
1776262004 JH5—May 9, 2004Kitt PeakSpacewatchHYG3.6 kmMPC · JPL
1776272004 JO11—May 13, 2004SocorroLINEAR · 3.7 kmMPC · JPL
1776282004 JA12—May 13, 2004PalomarNEAT · 2.7 kmMPC · JPL
1776292004 JM25—May 15, 2004SocorroLINEARLIX6.4 kmMPC · JPL
1776302004 JZ42—May 15, 2004SocorroLINEARHYG5.0 kmMPC · JPL
1776312004 JM44—May 15, 2004SocorroLINEAR · 1.5 kmMPC · JPL
1776322004 JS48—May 13, 2004Kitt PeakSpacewatch · 3.7 kmMPC · JPL
1776332004 JW54—May 10, 2004Kitt PeakSpacewatchHOF4.2 kmMPC · JPL
1776342004 KL4—May 16, 2004Siding SpringSSS · 3.3 kmMPC · JPL
1776352004 LQ3—June 11, 2004PalomarNEAT · 5.6 kmMPC · JPL
1776362004 LB9—June 13, 2004SocorroLINEAR · 4.6 kmMPC · JPL
1776372004 LY13—June 11, 2004SocorroLINEAREUN2.5 kmMPC · JPL
1776382004 LB22—June 13, 2004Kitt PeakSpacewatchEOS · 5.4 kmMPC · JPL
1776392004 LW28—June 14, 2004Kitt PeakSpacewatch · 4.3 kmMPC · JPL
1776402004 NX10—July 10, 2004CatalinaCSSHIL · 3:212 kmMPC · JPL
1776412004 NE20—July 14, 2004SocorroLINEARHYG3.2 kmMPC · JPL
1776422004 NU27—July 11, 2004SocorroLINEAR · 6.4 kmMPC · JPL
1776432004 OO4—July 16, 2004SocorroLINEAR · 4.7 kmMPC · JPL
1776442004 PN88—August 11, 2004PalomarNEATEUP6.7 kmMPC · JPL
1776452004 PQ89—August 9, 2004Campo ImperatoreCINEOS · 3.3 kmMPC · JPL
1776462004 RK80—September 8, 2004SocorroLINEAR · 4.6 kmMPC · JPL
1776472004 RF110—September 6, 2004SocorroLINEARH990 mMPC · JPL
1776482004 RR179—September 10, 2004SocorroLINEAR · 4.0 kmMPC · JPL
1776492004 TP8—October 6, 2004SocorroLINEARH1.5 kmMPC · JPL
1776502004 VN75—November 4, 2004SocorroLINEARH920 mMPC · JPL
1776512004 XM14—December 10, 2004CatalinaCSSAPO +1km1.1 kmMPC · JPL
1776522004 XW130—December 15, 2004CatalinaCSSH880 mMPC · JPL
1776532004 XM155—December 12, 2004Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1776542004 YR33—December 16, 2004CatalinaCSSH1.1 kmMPC · JPL
1776552005 AF32—January 11, 2005SocorroLINEARL519 kmMPC · JPL
1776562005 CU6—February 2, 2005CatalinaCSSH1.0 kmMPC · JPL
1776572005 CN21—February 2, 2005CatalinaCSSNYS1.0 kmMPC · JPL
1776582005 CJ74—February 1, 2005Kitt PeakSpacewatch · 2.3 kmMPC · JPL
177659 Paolacel2005 CE77PaolacelFebruary 9, 2005La SillaA. Boattini, H. Scholl · 1.3 kmMPC · JPL
1776602005 EJ2—March 3, 2005SocorroLINEARH1.4 kmMPC · JPL
1776612005 EK5—March 1, 2005Kitt PeakSpacewatchNYS870 mMPC · JPL
1776622005 EM5—March 1, 2005Kitt PeakSpacewatchNYS900 mMPC · JPL
1776632005 EC6—March 1, 2005Kitt PeakSpacewatchNYS1.1 kmMPC · JPL | 31 | 10 |
1776642005 EH11—March 2, 2005CatalinaCSS · 1.1 kmMPC · JPL
1776652005 EV34—March 3, 2005Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1776662005 EW34—March 3, 2005CatalinaCSSNYS830 mMPC · JPL
177667 Schieven2005 EV37SchievenMarch 3, 2005JarnacJarnac Obs. · 1.1 kmMPC · JPL
1776682005 EL42—March 2, 2005CatalinaCSSH1.1 kmMPC · JPL
1776692005 EK46—March 3, 2005CatalinaCSSNYS2.4 kmMPC · JPL
1776702005 EM50—March 3, 2005CatalinaCSSNYS860 mMPC · JPL
1776712005 EX51—March 3, 2005Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1776722005 EQ58—March 4, 2005Kitt PeakSpacewatchNYS840 mMPC · JPL
1776732005 EV68—March 7, 2005SocorroLINEAR · 1.0 kmMPC · JPL
1776742005 EF88—March 7, 2005Siding SpringSSS · 1.5 kmMPC · JPL
1776752005 ED98—March 3, 2005CatalinaCSSV960 mMPC · JPL
1776762005 EG130—March 9, 2005Mount LemmonMount Lemmon SurveyV980 mMPC · JPL
1776772005 EX138—March 9, 2005Mount LemmonMount Lemmon Survey · 1.4 kmMPC · JPL
1776782005 EK205—March 12, 2005Mount LemmonMount Lemmon Survey · 1.3 kmMPC · JPL
1776792005 EM205—March 12, 2005Kitt PeakSpacewatch · 940 mMPC · JPL
1776802005 ES216—March 8, 2005Mount LemmonMount Lemmon Survey · 850 mMPC · JPL
1776812005 ES223—March 12, 2005Kitt PeakSpacewatchFLO740 mMPC · JPL
1776822005 ED232—March 10, 2005Mount LemmonMount Lemmon Survey · 1.0 kmMPC · JPL
1776832005 EE234—March 10, 2005Anderson MesaLONEOS · 1.2 kmMPC · JPL
1776842005 EJ253—March 11, 2005Anderson MesaLONEOS · 1.1 kmMPC · JPL
1776852005 EE264—March 13, 2005Kitt PeakSpacewatchERI2.1 kmMPC · JPL
1776862005 EU265—March 13, 2005CatalinaCSS · 1.1 kmMPC · JPL
1776872005 EX267—March 14, 2005Mount LemmonMount Lemmon Survey · 1.0 kmMPC · JPL
1776882005 EY279—March 10, 2005CatalinaCSSV870 mMPC · JPL
1776892005 EX323—March 11, 2005Mount LemmonMount Lemmon SurveyNYS900 mMPC · JPL
1776902005 FX2—March 16, 2005Goodricke-PigottR. A. TuckerNYS940 mMPC · JPL
1776912005 GV3—April 1, 2005Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1776922005 GO6—April 1, 2005Kitt PeakSpacewatchNYS700 mMPC · JPL
1776932005 GW6—April 1, 2005Kitt PeakSpacewatchNYS710 mMPC · JPL
1776942005 GH11—April 1, 2005Anderson MesaLONEOSV930 mMPC · JPL
1776952005 GM20—April 2, 2005Mount LemmonMount Lemmon Survey · 1.3 kmMPC · JPL
1776962005 GA23—April 1, 2005Anderson MesaLONEOS · 1.2 kmMPC · JPL
1776972005 GF23—April 1, 2005Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1776982005 GW26—April 2, 2005Anderson MesaLONEOSFLO1.0 kmMPC · JPL
1776992005 GJ29—April 4, 2005Kitt PeakSpacewatchFLO770 mMPC · JPL
1777002005 GL51—April 2, 2005Mount LemmonMount Lemmon SurveyV990 mMPC · JPL
177701–177800
back to top
Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1777012005 GM66—April 2, 2005Mount LemmonMount Lemmon Survey · 1.8 kmMPC · JPL
1777022005 GS70—April 4, 2005Kitt PeakSpacewatchNYS1.4 kmMPC · JPL
1777032005 GU71—April 4, 2005CatalinaCSS · 1.0 kmMPC · JPL
1777042005 GU73—April 4, 2005CatalinaCSS · 1.2 kmMPC · JPL
1777052005 GK79—April 6, 2005Mount LemmonMount Lemmon Survey · 1.0 kmMPC · JPL
1777062005 GE90—April 6, 2005Kitt PeakSpacewatchFLO980 mMPC · JPL
1777072005 GV93—April 6, 2005Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1777082005 GQ103—April 9, 2005Mount LemmonMount Lemmon Survey · 830 mMPC · JPL
1777092005 GD123—April 6, 2005Mount LemmonMount Lemmon SurveyMAS1.0 kmMPC · JPL
1777102005 GM125—April 10, 2005Mount LemmonMount Lemmon SurveyNYS940 mMPC · JPL
1777112005 GW127—April 9, 2005SocorroLINEAR · 1.1 kmMPC · JPL
1777122005 GJ139—April 12, 2005Mount LemmonMount Lemmon SurveyFLO760 mMPC · JPL
1777132005 GZ140—April 14, 2005Reedy CreekJ. Broughton · 2.8 kmMPC · JPL
1777142005 GZ145—April 11, 2005Kitt PeakSpacewatch · 920 mMPC · JPL
1777152005 GN154—April 9, 2005SocorroLINEAR · 1.0 kmMPC · JPL
1777162005 GH160—April 12, 2005Kitt PeakSpacewatch · 960 mMPC · JPL
1777172005 GB161—April 13, 2005SocorroLINEAR · 1.7 kmMPC · JPL
1777182005 GS161—April 13, 2005CatalinaCSS · 2.0 kmMPC · JPL
1777192005 GD167—April 11, 2005Mount LemmonMount Lemmon Survey · 1.3 kmMPC · JPL
1777202005 GA175—April 14, 2005Kitt PeakSpacewatch · 980 mMPC · JPL
1777212005 GM202—April 5, 2005Kitt PeakSpacewatch · 1.0 kmMPC · JPL
177722 Pelletier2005 GJ205PelletierApril 11, 2005Kitt PeakM. W. Buie · 990 mMPC · JPL
1777232005 GY214—April 7, 2005Kitt PeakSpacewatch · 990 mMPC · JPL
1777242005 GZ223—April 12, 2005Siding SpringSSS · 2.2 kmMPC · JPL
1777252005 HM1—April 16, 2005Kitt PeakSpacewatch · 1.7 kmMPC · JPL | 31 | 11 |
1777262005 HX4—April 30, 2005Kitt PeakSpacewatch · 1.3 kmMPC · JPL
1777272005 JP—May 3, 2005Kitt PeakSpacewatchMAS1.2 kmMPC · JPL
1777282005 JE3—May 3, 2005CatalinaCSSNYS1.0 kmMPC · JPL
1777292005 JL4—May 3, 2005SocorroLINEAR · 3.2 kmMPC · JPL
1777302005 JM4—May 3, 2005CatalinaCSS · 1.9 kmMPC · JPL
1777312005 JK17—May 4, 2005CatalinaCSSFLO850 mMPC · JPL
1777322005 JZ20—May 4, 2005PalomarNEATKOR2.1 kmMPC · JPL
1777332005 JO21—May 4, 2005Siding SpringSSSNYS870 mMPC · JPL
1777342005 JV22—May 1, 2005PalomarNEAT · 1.3 kmMPC · JPL
1777352005 JC25—May 3, 2005Kitt PeakSpacewatchV980 mMPC · JPL
1777362005 JH25—May 3, 2005Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1777372005 JK27—May 3, 2005SocorroLINEARFLO1.1 kmMPC · JPL
1777382005 JT31—May 4, 2005Anderson MesaLONEOSFLO940 mMPC · JPL
1777392005 JD38—May 6, 2005SocorroLINEAR · 2.0 kmMPC · JPL
1777402005 JE38—May 6, 2005HaleakalaNEAT · 1.4 kmMPC · JPL
1777412005 JM42—May 8, 2005Anderson MesaLONEOS · 1.1 kmMPC · JPL
1777422005 JR42—May 8, 2005Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1777432005 JA43—May 8, 2005SocorroLINEAR · 1.6 kmMPC · JPL
1777442005 JG44—May 4, 2005Siding SpringSSS · 1.4 kmMPC · JPL
1777452005 JM44—May 8, 2005Mount LemmonMount Lemmon Survey · 1.2 kmMPC · JPL
1777462005 JU54—May 4, 2005Mount LemmonMount Lemmon SurveyV1.1 kmMPC · JPL
1777472005 JR55—May 4, 2005PalomarNEAT · 1.4 kmMPC · JPL
1777482005 JQ64—May 4, 2005PalomarNEAT · 2.9 kmMPC · JPL
1777492005 JU69—May 7, 2005Kitt PeakSpacewatch · 1.8 kmMPC · JPL
1777502005 JH73—May 8, 2005Kitt PeakSpacewatchV1.1 kmMPC · JPL
1777512005 JB75—May 8, 2005Siding SpringSSS · 1.5 kmMPC · JPL
1777522005 JR75—May 9, 2005Anderson MesaLONEOSFLO950 mMPC · JPL
1777532005 JC84—May 8, 2005Kitt PeakSpacewatchNYS690 mMPC · JPL
1777542005 JE86—May 8, 2005Mount LemmonMount Lemmon SurveyMAS950 mMPC · JPL
1777552005 JT90—May 11, 2005PalomarNEATFLO1.0 kmMPC · JPL
1777562005 JV90—May 11, 2005Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1777572005 JE92—May 11, 2005PalomarNEAT · 1.5 kmMPC · JPL
1777582005 JK93—May 11, 2005PalomarNEAT · 1.3 kmMPC · JPL
1777592005 JL107—May 12, 2005Mount LemmonMount Lemmon Survey · 1.4 kmMPC · JPL
1777602005 JP109—May 12, 2005CatalinaCSSADE3.5 kmMPC · JPL
1777612005 JU120—May 10, 2005Kitt PeakSpacewatch · 1.8 kmMPC · JPL
1777622005 JF124—May 11, 2005Mount LemmonMount Lemmon SurveyNYS830 mMPC · JPL
1777632005 JG125—May 11, 2005PalomarNEAT · 2.0 kmMPC · JPL
1777642005 JB127—May 12, 2005Mount LemmonMount Lemmon SurveyNYS1.2 kmMPC · JPL
1777652005 JM127—May 12, 2005SocorroLINEAR · 1.2 kmMPC · JPL
1777662005 JB128—May 12, 2005Kitt PeakSpacewatchRAF1.6 kmMPC · JPL
1777672005 JR128—May 13, 2005Kitt PeakSpacewatchFLO980 mMPC · JPL
1777682005 JX137—May 13, 2005Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1777692005 JZ145—May 13, 2005Mount LemmonMount Lemmon Survey · 1.4 kmMPC · JPL
177770 Saulanwu2005 JE163SaulanwuMay 8, 2005Mount LemmonMount Lemmon Survey · 2.0 kmMPC · JPL
177771 Bretz2005 JA165BretzMay 10, 2005Mount LemmonMount Lemmon Survey · 1.7 kmMPC · JPL
1777722005 JJ168—May 8, 2005Mount LemmonMount Lemmon Survey · 1.7 kmMPC · JPL
1777732005 JT176—May 12, 2005Anderson MesaLONEOS · 1.5 kmMPC · JPL
1777742005 KD1—May 16, 2005Kitt PeakSpacewatchV1.0 kmMPC · JPL
1777752005 KB2—May 16, 2005Mount LemmonMount Lemmon SurveyV1.1 kmMPC · JPL
1777762005 KJ5—May 18, 2005Siding SpringSSS · 960 mMPC · JPL
1777772005 KM6—May 18, 2005PalomarNEAT · 870 mMPC · JPL
1777782005 KX6—May 19, 2005Mount LemmonMount Lemmon SurveyNYS1.0 kmMPC · JPL
1777792005 KP8—May 18, 2005Siding SpringSSS · 1.1 kmMPC · JPL
1777802005 KK10—May 29, 2005Siding SpringSSSNYS1.2 kmMPC · JPL
1777812005 KJ13—May 22, 2005PalomarNEATNYS1.1 kmMPC · JPL
1777822005 LG1—June 3, 2005Reedy CreekJ. BroughtonNYS950 mMPC · JPL
1777832005 LF2—June 2, 2005CatalinaCSS · 950 mMPC · JPL
1777842005 LY9—June 2, 2005Siding SpringSSSERI2.2 kmMPC · JPL
1777852005 LH12—June 5, 2005SocorroLINEARFLO970 mMPC · JPL
1777862005 LQ15—June 5, 2005SocorroLINEAR · 970 mMPC · JPL
1777872005 LB18—June 6, 2005Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1777882005 LB19—June 8, 2005Kitt PeakSpacewatch · 1.2 kmMPC · JPL | 31 | 12 |
1777892005 LH19—June 8, 2005Kitt PeakSpacewatch · 2.3 kmMPC · JPL
1777902005 LD21—June 5, 2005SocorroLINEARNYS1.1 kmMPC · JPL
1777912005 LJ22—June 8, 2005Kitt PeakSpacewatchFLO970 mMPC · JPL
1777922005 LW22—June 8, 2005Kitt PeakSpacewatch · 3.4 kmMPC · JPL
1777932005 LH24—June 6, 2005Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1777942005 LS25—June 8, 2005Kitt PeakSpacewatch · 2.4 kmMPC · JPL
1777952005 LH27—June 9, 2005Kitt PeakSpacewatch · 1.0 kmMPC · JPL
1777962005 LO35—June 10, 2005Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1777972005 LJ39—June 11, 2005Kitt PeakSpacewatch · 4.3 kmMPC · JPL
1777982005 LR45—June 13, 2005Mount LemmonMount Lemmon SurveyMIS3.1 kmMPC · JPL
1777992005 LW45—June 13, 2005Kitt PeakSpacewatch · 2.1 kmMPC · JPL
1778002005 LT49—June 11, 2005CatalinaCSSFLO980 mMPC · JPL
177801–177900
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Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1778012005 LA50—June 11, 2005Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1778022005 LP50—June 13, 2005Mount LemmonMount Lemmon SurveyNYS1.2 kmMPC · JPL
1778032005 LX50—June 13, 2005Mount LemmonMount Lemmon Survey · 4.0 kmMPC · JPL
1778042005 LW52—June 1, 2005Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1778052005 LC53—June 1, 2005Kitt PeakSpacewatchV1.1 kmMPC · JPL
1778062005 MU—June 17, 2005Mount LemmonMount Lemmon Survey · 3.3 kmMPC · JPL
1778072005 MF1—June 17, 2005Mount LemmonMount Lemmon SurveyEOS2.6 kmMPC · JPL
1778082005 MF2—June 16, 2005Kitt PeakSpacewatchGEF2.2 kmMPC · JPL
1778092005 MO2—June 17, 2005Kitt PeakSpacewatchMAR1.6 kmMPC · JPL
1778102005 MW8—June 28, 2005Kitt PeakSpacewatch · 2.2 kmMPC · JPL
1778112005 MN12—June 28, 2005PalomarNEATHYG4.7 kmMPC · JPL
1778122005 MU16—June 27, 2005Kitt PeakSpacewatch · 2.0 kmMPC · JPL
1778132005 MC17—June 27, 2005Kitt PeakSpacewatch · 2.8 kmMPC · JPL
1778142005 ME17—June 27, 2005Kitt PeakSpacewatchTHM4.0 kmMPC · JPL
1778152005 MJ21—June 30, 2005PalomarNEAT · 1.3 kmMPC · JPL
1778162005 MK24—June 30, 2005Kitt PeakSpacewatch · 3.5 kmMPC · JPL
1778172005 MB31—June 30, 2005Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1778182005 MA35—June 30, 2005Kitt PeakSpacewatch · 3.4 kmMPC · JPL
1778192005 MW43—June 27, 2005PalomarNEAT · 1.4 kmMPC · JPL
1778202005 MG53—June 29, 2005PalomarNEAT · 3.5 kmMPC · JPL
1778212005 NL3—July 1, 2005Kitt PeakSpacewatchTIR5.1 kmMPC · JPL
1778222005 NQ12—July 4, 2005Mount LemmonMount Lemmon SurveyEOS2.6 kmMPC · JPL
1778232005 NB13—July 4, 2005PalomarNEAT · 4.3 kmMPC · JPL
1778242005 NB15—July 6, 2005Junk BondD. HealyMAS1.0 kmMPC · JPL
1778252005 NM16—July 2, 2005Kitt PeakSpacewatchHEN1.4 kmMPC · JPL
1778262005 NM18—July 4, 2005Mount LemmonMount Lemmon SurveyHYG3.4 kmMPC · JPL
1778272005 NY18—July 4, 2005Mount LemmonMount Lemmon Survey · 3.1 kmMPC · JPL
1778282005 NS36—July 6, 2005Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1778292005 NC43—July 5, 2005PalomarNEATEOS2.6 kmMPC · JPL
177830 Rubenhagen2005 NL44RubenhagenJuly 9, 2005JarnacJarnac Obs. · 6.1 kmMPC · JPL
1778312005 NQ47—July 7, 2005Kitt PeakSpacewatch · 2.5 kmMPC · JPL
1778322005 NX50—July 6, 2005Kitt PeakSpacewatch · 3.0 kmMPC · JPL
1778332005 NJ52—July 10, 2005CatalinaCSSNYS1.2 kmMPC · JPL
1778342005 NW55—July 11, 2005RASA. LoweTHB5.6 kmMPC · JPL
1778352005 NM59—July 9, 2005Kitt PeakSpacewatch · 2.9 kmMPC · JPL
1778362005 NU65—July 1, 2005Kitt PeakSpacewatchKOR1.8 kmMPC · JPL
1778372005 NU69—July 4, 2005PalomarNEATVER4.4 kmMPC · JPL
1778382005 NZ69—July 4, 2005Mount LemmonMount Lemmon SurveyEOS3.1 kmMPC · JPL
1778392005 NB73—July 8, 2005Kitt PeakSpacewatch · 1.6 kmMPC · JPL
1778402005 NR75—July 10, 2005Kitt PeakSpacewatchNYS1.1 kmMPC · JPL
1778412005 ND80—July 10, 2005Reedy CreekJ. BroughtonEOS3.3 kmMPC · JPL
1778422005 NA96—July 7, 2005Kitt PeakSpacewatch · 2.4 kmMPC · JPL
1778432005 NJ122—July 5, 2005PalomarNEAT · 3.0 kmMPC · JPL
1778442005 NL122—July 12, 2005Mount LemmonMount Lemmon Survey · 3.9 kmMPC · JPL
1778452005 OZ9—July 27, 2005PalomarNEAT · 4.8 kmMPC · JPL
1778462005 OD10—July 27, 2005PalomarNEAT · 5.2 kmMPC · JPL
1778472005 OV18—July 30, 2005PalomarNEAT · 2.9 kmMPC · JPL
1778482005 OV19—July 28, 2005PalomarNEAT · 3.6 kmMPC · JPL
1778492005 OG24—July 30, 2005PalomarNEAT · 4.3 kmMPC · JPL | 31 | 13 |
1778502005 OM24—July 30, 2005PalomarNEAT · 3.7 kmMPC · JPL
1778512005 OC26—July 28, 2005PalomarNEAT · 2.9 kmMPC · JPL
1778522005 OZ26—July 30, 2005PalomarNEAT · 4.5 kmMPC · JPL
177853 Lumezzane2005 PQ3LumezzaneAugust 5, 2005LumezzaneM. Micheli, G. P. Pizzetti · 1.7 kmMPC · JPL
1778542005 PY5—August 4, 2005KingsnakeJ. V. McClusky · 5.0 kmMPC · JPL
1778552005 PL19—August 5, 2005PalomarNEAT · 3.5 kmMPC · JPL
1778562005 PN19—August 5, 2005PalomarNEATHOF4.2 kmMPC · JPL
1778572005 PP19—August 5, 2005PalomarNEAT · 4.6 kmMPC · JPL
1778582005 QX—August 22, 2005PalomarNEATEOS3.1 kmMPC · JPL
1778592005 QB3—August 24, 2005PalomarNEAT · 4.2 kmMPC · JPL
1778602005 QG3—August 24, 2005PalomarNEATEOS3.0 kmMPC · JPL
1778612005 QM9—August 25, 2005PalomarNEATHYG3.8 kmMPC · JPL
1778622005 QE13—August 24, 2005PalomarNEAT · 4.3 kmMPC · JPL
1778632005 QE16—August 25, 2005PalomarNEATEOS2.5 kmMPC · JPL
1778642005 QG19—August 25, 2005Campo ImperatoreCINEOSTEL2.0 kmMPC · JPL
1778652005 QU20—August 26, 2005Anderson MesaLONEOS · 2.8 kmMPC · JPL
1778662005 QL28—August 28, 2005VicquesM. OryHOF3.8 kmMPC · JPL
1778672005 QV31—August 24, 2005PalomarNEATHYG3.9 kmMPC · JPL
1778682005 QR33—August 25, 2005PalomarNEATKOR2.0 kmMPC · JPL
1778692005 QN45—August 26, 2005PalomarNEATURS5.9 kmMPC · JPL
1778702005 QR46—August 26, 2005PalomarNEAT · 4.7 kmMPC · JPL
1778712005 QQ48—August 26, 2005PalomarNEAT · 5.2 kmMPC · JPL
1778722005 QV58—August 25, 2005PalomarNEATHYG4.9 kmMPC · JPL
1778732005 QR70—August 29, 2005SocorroLINEAREOS3.7 kmMPC · JPL
1778742005 QM74—August 29, 2005Anderson MesaLONEOS · 4.4 kmMPC · JPL
1778752005 QS78—August 25, 2005PalomarNEAT · 4.1 kmMPC · JPL
1778762005 QW83—August 29, 2005Anderson MesaLONEOS · 4.3 kmMPC · JPL
1778772005 QB95—August 27, 2005PalomarNEAT · 3.7 kmMPC · JPL
1778782005 QO101—August 27, 2005PalomarNEATEOS3.0 kmMPC · JPL
1778792005 QH104—August 27, 2005PalomarNEAT7:44.6 kmMPC · JPL
1778802005 QD109—August 27, 2005PalomarNEATCHA3.6 kmMPC · JPL
1778812005 QA113—August 27, 2005PalomarNEAT · 4.9 kmMPC · JPL
1778822005 QH113—August 27, 2005PalomarNEAT · 3.6 kmMPC · JPL
1778832005 QA119—August 28, 2005Kitt PeakSpacewatch · 3.4 kmMPC · JPL
1778842005 QS124—August 28, 2005Kitt PeakSpacewatch · 3.2 kmMPC · JPL
1778852005 QD137—August 28, 2005Kitt PeakSpacewatchHYG4.0 kmMPC · JPL
1778862005 QN138—August 28, 2005Kitt PeakSpacewatch · 5.9 kmMPC · JPL
1778872005 QC141—August 29, 2005Anderson MesaLONEOS · 3.7 kmMPC · JPL
1778882005 QE142—August 30, 2005SocorroLINEAR · 7.2 kmMPC · JPL
1778892005 QZ143—August 26, 2005PalomarNEAT · 5.1 kmMPC · JPL
1778902005 QP146—August 28, 2005Siding SpringSSS · 4.6 kmMPC · JPL
1778912005 QK159—August 28, 2005Anderson MesaLONEOS · 4.8 kmMPC · JPL
1778922005 QE163—August 30, 2005Anderson MesaLONEOS · 3.9 kmMPC · JPL
1778932005 QP170—August 29, 2005PalomarNEAT · 5.0 kmMPC · JPL
1778942005 QY177—August 31, 2005PalomarNEATHYG3.1 kmMPC · JPL
1778952005 QU178—August 29, 2005Anderson MesaLONEOS7:46.0 kmMPC · JPL
1778962005 RD6—September 6, 2005SocorroLINEAR · 5.2 kmMPC · JPL
1778972005 RK6—September 7, 2005AltschwendtAltschwendt Obs. · 5.6 kmMPC · JPL
1778982005 RX7—September 8, 2005SocorroLINEAR3:26.8 kmMPC · JPL
1778992005 RG23—September 9, 2005SocorroLINEAR · 5.3 kmMPC · JPL
1779002005 RS30—September 11, 2005Kitt PeakSpacewatch · 4.1 kmMPC · JPL
177901–178000
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Designation Discovery Properties Ref
Permanent Provisional Citation Date Site Discoverer(s) Category Diam.
1779012005 RZ37—September 3, 2005Mauna KeaC. VeilletVER5.3 kmMPC · JPL
1779022005 RG40—September 6, 2005Anderson MesaLONEOSEOS3.5 kmMPC · JPL
1779032005 RD41—September 12, 2005Kitt PeakSpacewatch · 3.4 kmMPC · JPL
1779042005 SV5—September 23, 2005CatalinaCSS · 5.8 kmMPC · JPL
1779052005 SA11—September 23, 2005Kitt PeakSpacewatchHYG4.2 kmMPC · JPL
1779062005 SO19—September 25, 2005Calvin-RehobothCalvin–Rehoboth Obs. · 3.6 kmMPC · JPL
1779072005 SF67—September 27, 2005Kitt PeakSpacewatch · 5.5 kmMPC · JPL
1779082005 SN77—September 24, 2005Kitt PeakSpacewatchKAR1.9 kmMPC · JPL
1779092005 SX96—September 25, 2005PalomarNEAT · 3.9 kmMPC · JPL | 31 | 14 |
1779102005 SA114—September 27, 2005Kitt PeakSpacewatch · 4.4 kmMPC · JPL
1779112005 SF117—September 28, 2005PalomarNEAT · 5.0 kmMPC · JPL
1779122005 SO122—September 29, 2005PalomarNEAT · 4.7 kmMPC · JPL
1779132005 SN139—September 25, 2005Kitt PeakSpacewatch · 4.5 kmMPC · JPL
1779142005 SX142—September 25, 2005Kitt PeakSpacewatch · 2.1 kmMPC · JPL
1779152005 SQ159—September 26, 2005PalomarNEAT · 5.5 kmMPC · JPL
1779162005 SY166—September 28, 2005PalomarNEAT · 5.0 kmMPC · JPL
1779172005 SY178—September 29, 2005Anderson MesaLONEOS · 4.7 kmMPC · JPL
1779182005 SL181—September 29, 2005Mount LemmonMount Lemmon Survey · 4.4 kmMPC · JPL
1779192005 SN190—September 29, 2005Anderson MesaLONEOSVER6.7 kmMPC · JPL
1779202005 SG225—September 29, 2005PalomarNEAT7:46.5 kmMPC · JPL
1779212005 SE233—September 30, 2005Mount LemmonMount Lemmon Survey · 5.3 kmMPC · JPL
1779222005 SD244—September 30, 2005Mount LemmonMount Lemmon SurveyEOS2.6 kmMPC · JPL
1779232005 SL245—September 30, 2005Mount LemmonMount Lemmon SurveyTHM3.5 kmMPC · JPL
1779242005 SV246—September 30, 2005Kitt PeakSpacewatchHYG4.4 kmMPC · JPL
1779252005 SV252—September 24, 2005PalomarNEAT · 6.6 kmMPC · JPL
1779262005 SP258—September 23, 2005CatalinaCSSEOS2.7 kmMPC · JPL
1779272005 SP259—September 25, 2005CatalinaCSSEOS4.1 kmMPC · JPL
1779282005 SK260—September 23, 2005Kitt PeakSpacewatchEOS2.5 kmMPC · JPL
1779292005 TE2—October 1, 2005CatalinaCSSMRX1.7 kmMPC · JPL
1779302005 TH43—October 5, 2005SocorroLINEAR · 3.6 kmMPC · JPL
1779312005 TD56—October 1, 2005Kitt PeakSpacewatch · 5.3 kmMPC · JPL
1779322005 TW73—October 7, 2005Anderson MesaLONEOS · 5.2 kmMPC · JPL
1779332005 TR75—October 3, 2005CatalinaCSS · 2.6 kmMPC · JPL
1779342005 TQ101—October 7, 2005CatalinaCSS · 4.7 kmMPC · JPL
1779352005 TS111—October 7, 2005Kitt PeakSpacewatchHYG3.8 kmMPC · JPL
1779362005 UD10—October 21, 2005PalomarNEAT · 4.8 kmMPC · JPL
1779372005 UD49—October 23, 2005CatalinaCSS · 6.9 kmMPC · JPL
1779382005 UJ121—October 24, 2005Kitt PeakSpacewatch · 4.6 kmMPC · JPL
1779392005 UV137—October 25, 2005Mount LemmonMount Lemmon Survey · 3.4 kmMPC · JPL
1779402005 UC144—October 26, 2005Kitt PeakSpacewatchSHU · 3:27.6 kmMPC · JPL
1779412005 UR265—October 27, 2005Kitt PeakSpacewatch3:26.7 kmMPC · JPL
1779422005 VP17—November 4, 2005Mount LemmonMount Lemmon Survey · 5.6 kmMPC · JPL
1779432005 VZ17—November 1, 2005Kitt PeakSpacewatchSHU · 3:210 kmMPC · JPL
1779442005 VM64—November 1, 2005Mount LemmonMount Lemmon Survey · 3.7 kmMPC · JPL
1779452005 WO60—November 25, 2005PalomarNEAT · 4.7 kmMPC · JPL
1779462005 WG68—November 25, 2005Mount LemmonMount Lemmon Survey · 4.9 kmMPC · JPL
1779472006 JS6—May 1, 2006Kitt PeakSpacewatch · 1.2 kmMPC · JPL
1779482006 KV—May 18, 2006PalomarNEATNYS910 mMPC · JPL
1779492006 KU96—May 25, 2006Kitt PeakSpacewatchV1.2 kmMPC · JPL
1779502006 KW96—May 25, 2006Mount LemmonMount Lemmon SurveyFLO920 mMPC · JPL
1779512006 KM114—May 24, 2006CatalinaCSSH1.1 kmMPC · JPL
1779522006 KX123—May 25, 2006CatalinaCSS · 2.1 kmMPC · JPL
1779532006 MQ6—June 20, 2006CatalinaCSS · 1.3 kmMPC · JPL
1779542006 OA—July 16, 2006EskridgeD. Tibbets, G. HugEUN1.8 kmMPC · JPL
1779552006 OP4—July 21, 2006Mount LemmonMount Lemmon Survey · 4.6 kmMPC · JPL
1779562006 OQ7—July 19, 2006PalomarNEATFLO1.1 kmMPC · JPL
1779572006 OC14—July 21, 2006PalomarNEAT · 1.0 kmMPC · JPL
1779582006 PX3—August 14, 2006Reedy CreekJ. Broughton · 1.3 kmMPC · JPL
1779592006 PP5—August 12, 2006PalomarNEAT · 780 mMPC · JPL
1779602006 PF7—August 12, 2006PalomarNEAT · 1.0 kmMPC · JPL
1779612006 PQ8—August 13, 2006PalomarNEAT · 1.4 kmMPC · JPL
1779622006 PN14—August 15, 2006PalomarNEAT · 3.5 kmMPC · JPL
1779632006 PR16—August 15, 2006PalomarNEAT · 1.2 kmMPC · JPL
1779642006 PE19—August 13, 2006PalomarNEAT · 840 mMPC · JPL
1779652006 PP22—August 14, 2006Siding SpringSSSV1.3 kmMPC · JPL
1779662006 PW22—August 15, 2006PalomarNEAT · 1.00 kmMPC · JPL
177967 Chouchihkang2006 PY32ChouchihkangAugust 15, 2006Lulin ObservatoryH.-C. Lin, Q.-z. YeV890 mMPC · JPL
1779682006 PK39—August 14, 2006PalomarNEAT · 2.4 kmMPC · JPL
1779692006 PM40—August 14, 2006PalomarNEAT · 1.5 kmMPC · JPL
1779702006 PC41—August 14, 2006PalomarNEAT · 1.7 kmMPC · JPL
1779712006 QC—August 17, 2006HibiscusS. | 31 | 15 |
F. Hönig · 1.0 kmMPC · JPL
1779722006 QL2—August 17, 2006PalomarNEAT · 2.9 kmMPC · JPL
1779732006 QO7—August 18, 2006Kitt PeakSpacewatch · 3.0 kmMPC · JPL
1779742006 QS8—August 19, 2006Kitt PeakSpacewatchV970 mMPC · JPL
1779752006 QR19—August 17, 2006PalomarNEATMAR1.7 kmMPC · JPL
1779762006 QR20—August 18, 2006Anderson MesaLONEOS · 1.6 kmMPC · JPL
1779772006 QV20—August 18, 2006Anderson MesaLONEOS · 3.2 kmMPC · JPL
1779782006 QE23—August 19, 2006PalomarNEAT · 1.3 kmMPC · JPL
1779792006 QV24—August 17, 2006PalomarNEATXIZ2.4 kmMPC · JPL
1779802006 QC28—August 20, 2006Kitt PeakSpacewatch · 1.4 kmMPC · JPL
1779812006 QO28—August 21, 2006SocorroLINEAR · 1.4 kmMPC · JPL
177982 Popilnia2006 QE34PopilniaAugust 17, 2006AndrushivkaAndrushivka Obs.NYS960 mMPC · JPL
1779832006 QE37—August 17, 2006PalomarNEAT · 5.3 kmMPC · JPL
1779842006 QU42—August 17, 2006PalomarNEAT · 1.2 kmMPC · JPL
1779852006 QV42—August 17, 2006PalomarNEATV960 mMPC · JPL
1779862006 QM43—August 18, 2006Kitt PeakSpacewatchMAS1.4 kmMPC · JPL
1779872006 QP43—August 18, 2006Kitt PeakSpacewatchNYS820 mMPC · JPL
1779882006 QV45—August 19, 2006Anderson MesaLONEOS · 2.8 kmMPC · JPL
1779892006 QX46—August 20, 2006PalomarNEATV1.2 kmMPC · JPL
1779902006 QP48—August 21, 2006SocorroLINEAR · 1.3 kmMPC · JPL
1779912006 QA49—August 21, 2006Kitt PeakSpacewatch · 980 mMPC · JPL
1779922006 QP56—August 21, 2006Kitt PeakSpacewatchDOR3.6 kmMPC · JPL
1779932006 QW57—August 24, 2006SocorroLINEAR · 9.1 kmMPC · JPL
1779942006 QP63—August 24, 2006SocorroLINEAR · 1.3 kmMPC · JPL
1779952006 QB66—August 28, 2006SocorroLINEARH1.0 kmMPC · JPL
1779962006 QT76—August 21, 2006Kitt PeakSpacewatch · 1.1 kmMPC · JPL
1779972006 QZ88—August 27, 2006Kitt PeakSpacewatch · 1.5 kmMPC · JPL
1779982006 QK113—August 24, 2006SocorroLINEARFLO950 mMPC · JPL
1779992006 QL115—August 27, 2006Anderson MesaLONEOS · 2.0 kmMPC · JPL
1780002006 QT117—August 27, 2006Anderson MesaLONEOS · 3.1 kmMPC · JPL
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See also
• Meanings of minor planet names: 177001–178000
References
1. "Small-Body Orbital Elements: Numbered Asteroids, ELEMENTS.NUMBR (64 MB)". NASA's Jet Propulsion Laboratory. November 2023.
2. "Data Available from the Minor Planet Center: Discovery circumstances of the numbered minor planets, NumberedMPs.txt (53 MB)". International Astronomical Union's Minor Planet Center. November 2023.
3. "Critical Lists of Asteroids". Lowell Observatory. November 2023.
External links
• Discovery Circumstances: Numbered Minor Planets (175001)–(180000) (IAU Minor Planet Center)
List of minor planets
1–25,000
• 1–1000
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• 5k
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25,001–50,000
• 25k
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• 49k
50,001–75,000
• 50k
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(181902) 1999 RD215
(181902) 1999 RD215 is a trans-Neptunian object of the scattered disc, approximately 148 kilometers in diameter. It was discovered on 6 September 1999, by American astronomers Chad Trujillo, Jane Luu, and David Jewitt at the Mauna Kea Observatories, Hawaii. [2][3]
(181902) 1999 RD215
Discovery[1][2]
Discovered byC. Trujillo
J. X. Luu
D. C. Jewitt
Discovery siteMauna Kea Obs.
Discovery date6 September 1999
Designations
MPC designation
(181902) 1999 RD215
Alternative designations
1999 RD215
Minor planet category
TNO[1] · SDO[3][4] · distant[2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 3[1] · 1[2]
Observation arc8.03 yr (2,933 days)
Aphelion204.40 AU
Perihelion37.541 AU
Semi-major axis
120.97 AU
Eccentricity0.6897
Orbital period (sidereal)
1330.58 yr (485,993 d)
Mean anomaly
7.8003°
Mean motion
0° 0m 2.52s / day
Inclination25.990°
Longitude of ascending node
210.32°
Argument of perihelion
137.86°
Physical characteristics
Mean diameter
147 km[4]
148 km[5]
Geometric albedo
0.08 (estimate)[5]
0.09 (estimate)[4]
Absolute magnitude (H)
7.4[1] · 7.6[5]
Orbit and classification
1999 RD215 orbits from the center of the Kuiper belt to well beyond into the scattered disc. It orbits the Sun at a distance of 37.5–204.4 AU once every 1330 years and 7 months (485,993 days; semi-major axis of 121 AU). Its orbit has an eccentricity of 0.69 and an inclination of 26° with respect to the ecliptic. [1] The body's observation arc begins with its official discovery observation. [2]
Diameter and albedo
According to the Johnston's Archive and Michael Brown, 1999 RD215 measures 147 and 148 kilometers in diameter, and its surface has an estimated albedo of 0.09 and 0.08, respectively. [4][5]
See also
• List of Solar System objects by greatest aphelion
References
1. "JPL Small-Body Database Browser: 181902 (1999 RD215)" (2007-09-17 last obs.). Jet Propulsion Laboratory. Retrieved 16 January 2018.
2. "181902 (1999 RD215)". Minor Planet Center. Retrieved 16 January 2018.
3. "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 16 January 2018.
4. Johnston, Wm. Robert (15 October 2017). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 16 January 2018.
5. Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 16 January 2018.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Discovery Circumstances: Numbered Minor Planets (180001)-(185000) – Minor Planet Center
• (181902) 1999 RD215 at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• (181902) 1999 RD215 at the JPL Small-Body Database
Minor planets navigator
• (181902) 1999 RD215
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Authority control databases
• JPL SBDB
• MPC | 32 | 0 |
(182294) 2001 KU76
(182294) 2001 KU76 (provisional designation 2001 KU76) is a trans-Neptunian object (TNO) that has a possible 6:11 resonance with Neptune. [2][3]
(182294) 2001 KU76
Discovery[1]
Discovered byBuie, M. W.
Discovery date24 May 2001
Designations
MPC designation
(182294) 2001 KU76
Minor planet category
Trans-Neptunian object
6:11 resonance? [2][3]
Orbital characteristics[1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 4
Observation arc2536 days (6.94 yr)
Aphelion52.656 AU (7.8772 Tm) (Q)
Perihelion37.693 AU (5.6388 Tm) (q)
Semi-major axis
45.175 AU (6.7581 Tm) (a)
Eccentricity0.16561 (e)
Orbital period (sidereal)
303.63 yr (110903 d)
Mean anomaly
354.46° (M)
Mean motion
0° 0m 11.686s / day (n)
Inclination10.637° (i)
Longitude of ascending node
44.987° (Ω)
Time of perihelion
≈ 6 December 2021[4]
±3 months
Argument of perihelion
204.39° (ω)
Earth MOID36.6816 AU (5.48749 Tm)
Jupiter MOID32.3615 AU (4.84121 Tm)
Physical characteristics
Dimensions211 km (assumed)[5]
Geometric albedo
0.09 (assumed)
Absolute magnitude (H)
6.6[1]
Assuming a generic TNO albedo of 0.09, it is about 211 km in diameter. [5] The assumed diameter of this object makes it a possible dwarf planet. [6]
Resonance
Simulations by Lykawka in 2007 show that 2001 KU76 may be librating in the 6:11 resonance with Neptune. [2] Buie classifies it as probably in resonance, although some possible orbits do not librate. [3] 2001 KU76 has a semi-major axis of 45 AU and an orbital period of about 302 years. [1]
It has been observed 29 times over 6 years and has an orbit quality code of 4. [1]
References
1. "JPL Small-Body Database Browser: 182294 (2001 KU76)" (2008-05-03 last obs). Retrieved 7 April 2016.
2. Lykawka, Patryk Sofia; Mukai, Tadashi (July 2007). "Dynamical classification of trans-neptunian objects: Probing their origin, evolution, and interrelation". Icarus. 189 (1): 213–232. Bibcode:2007Icar..189..213L. doi:10.1016/j.icarus.2007.01.001.
3. Buie, Marc W. "Orbit Fit and Astrometric record for 182294" (2008-05-03 using 29 observations). SwRI (Space Science Department). Retrieved 2009-02-06.
4. JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
5. Johnston, Wm. Robert (22 August 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 2009-02-06.
6. Brown, Michael E. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2011-10-18. Retrieved 2012-09-04.
External links
• (182294) 2001 KU76 at the JPL Small-Body Database
Minor planets navigator
• (182294) 2001 KU76
Small Solar System bodies
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Sednoids
• 90377 Sedna
• 2012 VP113
• 541132 Leleākūhonua
• 2021 RR205
Authority control databases
• JPL SBDB
• MPC | 33 | 0 |
1844 Susilva
1844 Susilva, provisional designation 1972 UB, is a stony Eoan asteroid from the outer region of the asteroid belt, approximately 22 kilometers in diameter. It was discovered on 30 October 1972, by Swiss astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland, and later named after a schoolfriend of the discoverer. [2][7]
1844 Susilva
Discovery[1]
Discovered byP. Wild
Discovery siteZimmerwald Obs.
Discovery date30 October 1972
Designations
MPC designation
(1844) Susilva
Named after
Susi Petit–Pierre
(friend of discoverer)[2]
Alternative designations
1972 UB · 1943 EU
1953 AA · 1959 GJ
Minor planet category
main-belt · Eos[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc64.40 yr (23,521 days)
Aphelion3.1714 AU
Perihelion2.8587 AU
Semi-major axis
3.0150 AU
Eccentricity0.0518
Orbital period (sidereal)
5.24 yr (1,912 days)
Mean anomaly
70.711°
Mean motion
0° 11m 17.88s / day
Inclination11.788°
Longitude of ascending node
99.365°
Argument of perihelion
73.564°
Physical characteristics
Dimensions19.022±0.232 km[4]
22.41 km (calculated)[3]
26.800±0.321 km[5]
Geometric albedo
0.118±0.011[5]
0.14 (assumed)[3]
0.2358±0.0545[4]
Spectral type
S[3]
Absolute magnitude (H)
10.8[4][5] · 11.0[1][3] · 11.49±0.44[6]
Classification and orbit
Susilva is a member of the Eos family, a collisional group of more than 4,000 asteroids, which are well known for mostly being of silicaceous composition. It orbits the Sun in the outer main-belt at a distance of 2.9–3.2 AU once every 5 years and 3 months (1,912 days). Its orbit has an eccentricity of 0.05 and an inclination of 12° with respect to the ecliptic. [1] First identified as 1943 EU at Turku Observatory, Susilva's first used observation was taken at Uccle Observatory in 1953, extending the body's observation arc by 19 years prior to its official discovery observation. [7]
Physical characteristics
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid measures between 19.0 and 26.8 kilometers in diameter, and its surface has an albedo of 0.118 to 0.236. [4][5] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.14, taken from 221 Eos, the family's largest member and namesake – and calculates a diameter of 22.4 kilometers based on an absolute magnitude of 11.0. [3] Susilva's rotation period has not yet been measured. [3]
Naming
The discoverer named a pair of asteroids after two of his former schoolmates, Susi and Helen, both from the small village of Wald, Zürich in Switzerland. This one was dedicated to Susi Petit–Pierre, while the subsequently numbered asteroid, 1845 Helewalda, was given to Helen Gachnang. [2][8] The official naming citation was published by the Minor Planet Center on 18 April 1977 (M.P.C. 4156). [9]
References
1. "JPL Small-Body Database Browser: 1844 Susilva (1972 UB)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Archived from the original on 18 September 2020. Retrieved 1 July 2017.
2. Schmadel, Lutz D. (2007). "(1844) Susilva". Dictionary of Minor Planet Names – (1844) Susilva. Springer Berlin Heidelberg. p. 148. doi:10.1007/978-3-540-29925-7_1845. ISBN 978-3-540-00238-3.
3. "LCDB Data for (1844) Susilva". Asteroid Lightcurve Database (LCDB). Retrieved 1 March 2016.
4. Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 1 March 2016.
5. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 1 March 2016.
6. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 1 March 2016.
7. "1844 Susilva (1972 UB)". Minor Planet Center. Retrieved 1 March 2016.
8. "Himmlischer Besuch auf der Sternwarte Eschenberg" (in German). Sternwarte Eschenberg. Retrieved 1 March 2016. Helen Gachnang and Susi Petit-Pierre visit the Eschenberg Observatory
9. Schmadel, Lutz D. "Appendix – Publication Dates of the MPCs". Dictionary of Minor Planet Names – Addendum to Fifth Edition (2006–2008). Springer Berlin Heidelberg. p. 221. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7.
External links
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
• 1844 Susilva at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
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(192642) 1999 RD32
(192642) 1999 RD32, provisional designation: 1999 RD32, is an asteroid and suspected contact binary on an eccentric orbit, classified as a large near-Earth object and potentially hazardous asteroid of the Apollo group, approximately 5 kilometers (3 miles) in diameter. It was discovered on 8 September 1999, at a magnitude of 18, by astronomers of the LINEAR program using its 1-meter telescope at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, United States. [3][2] The asteroid is likely of carbonaceous composition and has a rotation period of 17.08 hours. [4][lower-alpha 1]
(192642) 1999 RD32
Goldstone radar image showing the two lobes of suspected contact binary 1999 RD32.
Discovery[1][2][3]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date8 September 1999
Designations
MPC designation
(192642) 1999 RD32
Alternative designations
1999 RD32
Minor planet category
Apollo · NEO · PHA[1][3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc21.92 yr (8,007 days)
Aphelion4.6801 AU
Perihelion0.6093 AU
Semi-major axis
2.6447 AU
Eccentricity0.7696
Orbital period (sidereal)
4.30 yr (1,571 days)
Mean anomaly
89.009°
Mean motion
0° 13m 45.12s / day
Inclination6.7914°
Longitude of ascending node
310.04°
Argument of perihelion
299.89°
Earth MOID0.0495 AU · 19.3 LD
Jupiter MOID0.6702 AU
Physical characteristics
Mean diameter
1.63 km (calculated–dated)[4]
5 km (est.–radiometric)[5]
Synodic rotation period
17.08±0.03 h[6][lower-alpha 1]
17.1±0.5 h[7]
Geometric albedo
0.04 (est.–radiometric)[5]
0.20 (assumed–dated)[4]
Spectral type
C[4][5][8][9]
Absolute magnitude (H)
16.00[8] · 16.23±0.01[9] · 16.3[1][4]
Description
1999 RD32 orbits the Sun at a distance of 0.6–4.7 AU once every 4 years and 4 months (1,571 days; semi-major axis of 2.64 AU). Its orbit has a high eccentricity of 0.77 and an inclination of 7° with respect to the ecliptic. [1]
The asteroid's observation arc begins with a precovery taken at Palomar Observatory in January 1995. [3] It is known that 1999 RD32 passed 0.0093 AU (1,390,000 km; 860,000 mi) from Earth on 27 August 1969. [10] During the 1969 close approach the asteroid reached about apparent magnitude 8.8. [11] The similarly-sized 4179 Toutatis also reached that brightness in September 2004. It passed less than 0.007 AU (1,000,000 km; 650,000 mi) from asteroid 29 Amphitrite on 17 January 1939. [1]
Arecibo radar observations on 5–6 March 2012 showed that 1999 RD32 is approximately 5 kilometers (3 mi) in diameter[5] and has an estimated albedo of only 0.04. [5] Other sources calculate a smaller diameter of 1.63 kilometers based on a dated assumption, that the object is a stony rather than a carbonaceous asteroid. [4] The two visible lobes suggest that 1999 RD32 is a tight binary asteroid or contact binary. [5] About 10–15% of near-Earth asteroids larger than 200 meters are expected to be contact binary asteroids with two lobes in mutual contact. [12]
Close-approaches to Earth[10]
DateDistance from Earth
1969-08-270.0093 AU (1,390,000 km; 860,000 mi)
2012-03-140.1487 AU (22,250,000 km; 13,820,000 mi)
2042-03-110.1428 AU (21,360,000 km; 13,270,000 mi)
2046-09-040.1071 AU (16,020,000 km; 9,960,000 mi)
History of close approaches of large near-Earth objects since 1908 (A)
PHA Date Approach distance (lunar dist.) Abs.
mag
(H) Diameter (C)
(m) Ref (D)
Nomi-
nal(B) Mini-
mum Maxi-
mum
(33342) 1998 WT241908-12-163.5423.5373.54717.9556–1795data
(458732) 2011 MD51918-09-170.9110.9090.91317.9556–1795data
(7482) 1994 PC11933-01-172.9272.9272.92816.8749–1357data
69230 Hermes1937-10-301.9261.9261.92717.5668–2158data
69230 Hermes1942-04-261.6511.6511.65117.5668–2158data
(137108) 1999 AN101946-08-072.4322.4292.43517.9556–1795data
(33342) 1998 WT241956-12-163.5233.5233.52317.9556–1795data
(163243) 2002 FB31961-04-124.9034.9004.90616.41669–1695data
(192642) 1999 RD321969-08-273.6273.6253.63016.31161–3750data
(143651) 2003 QO1041981-05-182.7612.7602.76116.01333–4306data
2017 CH11992-06-054.6913.3916.03717.9556–1795data
(170086) 2002 XR141995-06-244.2594.2594.26018.0531–1714data
(33342) 1998 WT242001-12-164.8594.8594.85917.9556–1795data
4179 Toutatis2004-09-294.0314.0314.03115.32440–2450data
2014 JO252017-04-194.5734.5734.57317.8582–1879data
(137108) 1999 AN102027-08-071.0141.0101.01917.9556–1795data
(35396) 1997 XF112028-10-262.4172.4172.41816.9881–2845data
(154276) 2002 SY502071-10-303.4153.4123.41817.6714–1406data
(164121) 2003 YT12073-04-294.4094.4094.40916.21167–2267data
(385343) 2002 LV2076-08-044.1844.1834.18516.61011–3266data
(52768) 1998 OR22079-04-164.6114.6114.61215.81462–4721data
(33342) 1998 WT242099-12-184.9194.9194.91917.9556–1795data
(85182) 1991 AQ2130-01-274.1404.1394.14117.11100data
314082 Dryope2186-07-163.7092.9964.78617.5668–2158data
(137126) 1999 CF92192-08-214.9704.9674.97318.0531–1714data
(290772) 2005 VC2198-05-051.9511.7912.13417.6638–2061data
(A) List includes near-Earth approaches of less than 5 lunar distances (LD) of objects with H brighter than 18. | 35 | 0 |
(B) Nominal geocentric distance from the Earth's center to the object's center (Earth radius≈0.017 LD).
(C) Diameter: estimated, theoretical mean-diameter based on H and albedo range between X and Y.
(D) Reference: data source from the JPL SBDB, with AU converted into LD (1 AU≈390 LD)
(E) Color codes: unobserved at close approach observed during close approach upcoming approaches
Numbering and naming
This minor planet was numbered by the Minor Planet Center on 13 November 2008. [13] As of 2018, it has not been named. [3]
Notes
1. Lightcurve plot of (192642) 1999 RD32, Palmer Divide Observatory, B. D. Warner (2012): rotation period 17.08±0.03 hours with a brightness amplitude of 0.28±0.02 mag. Summary figures at the LCDB
References
1. "JPL Small-Body Database Browser: 192642 (1999 RD32)" (2016-12-04 last obs.). Jet Propulsion Laboratory. Retrieved 16 January 2018.
2. "MPEC 1999-R32 : 1999 RD32". IAU Minor Planet Center. 11 September 1999. Retrieved 28 February 2014. (J99R32D)
3. "192642 (1999 RD32)". Minor Planet Center. Retrieved 16 January 2018.
4. "LCDB Data for (192642)". Asteroid Lightcurve Database (LCDB). Retrieved 16 January 2018.
5. "(192642) 1999 RD32 Goldstone Radar Observations Planning". NASA/JPL Asteroid Radar Research. 12 March 2012. Retrieved 16 January 2018.
6. Warner, Brian D.; Megna, Ralph (July 2012). "Lightcurve Analysis of NEA (192642) 1999 RD32". The Minor Planet Bulletin. 39 (3): 154. Bibcode:2012MPBu...39..154W. ISSN 1052-8091. Retrieved 16 January 2018.
7. Vaduvescu, O.; Macias, A. Aznar; Tudor, V.; Predatu, M.; Galád, A.; Gajdos, S.; et al. (August 2017). "The EURONEAR Lightcurve Survey of Near Earth Asteroids". Earth. 120 (2): 41–100. Bibcode:2017EM&P..120...41V. doi:10.1007/s11038-017-9506-9. hdl:10316/80202. Retrieved 16 January 2018.
8. Carry, B.; Solano, E.; Eggl, S.; DeMeo, F. E. (April 2016). "Spectral properties of near-Earth and Mars-crossing asteroids using Sloan photometry". Icarus. 268: 340–354. arXiv:1601.02087. Bibcode:2016Icar..268..340C. doi:10.1016/j.icarus.2015.12.047. Retrieved 16 January 2018.
9. Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 16 January 2018.
10. "JPL Close-Approach Data: 192642 (1999 RD32)" (2012-11-03 last obs and observation arc=17.8 years). Retrieved 28 February 2014.
11. "1999RD32 Ephemerides for 25 August 1969 through 31 August 1969". NEODyS (Near Earth Objects – Dynamic Site). Retrieved 28 February 2014.
12. Michael Busch (12 March 2012). "Near-Earth Asteroids and Radar Speckle Tracking" (PDF). Retrieved 28 February 2014.
13. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.
External links
• Arecibo images from 2012
• Asteroid Lightcurve Database (LCDB), query form (info Archived 16 December 2017 at the Wayback Machine)
• Dictionary of Minor Planet Names, Google books
• Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
• (192642) 1999 RD32 at NeoDyS-2, Near Earth Objects—Dynamic Site
• Ephemerides · Observation prediction · Orbital info · MOID · Proper elements · Observational info · Close approaches · Physical info · Orbit animation
• RD32 (192642) 1999 RD32 at ESA–space situational awareness
• RD32&tab=eph Ephemerides · RD32&tab=obs Observations · RD32&tab=orbprop Orbit · RD32&tab=physprops Physical properties · RD32&tab=summary Summary
• (192642) 1999 RD32 at the JPL Small-Body Database
Minor planets navigator
• (192642) 1999 RD32
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19521 Chaos
19521 Chaos is a cubewano, a Kuiper-belt object not in resonance with any planet. Chaos was discovered in 1998 by the Deep Ecliptic Survey with Kitt Peak's 4 m telescope. Its albedo is 0.050+0.030
−0.016,[8] making it, with its absolute magnitude (H) of 4.8,[4] equivalent to a single spherical body 600+140
−130 km in diameter. [8]
19521 Chaos
19521 Chaos as imaged by the Hubble Space Telescope in September 2001
Discovery
Discovered byDeep Ecliptic Survey
Discovery date19 November 1998
Designations
MPC designation
(19521) Chaos
Pronunciation/ˈkeɪ.ɒs/
Named after
Chaos
Alternative designations
1998 WH24
Minor planet category
TNO (cubewano)[1][2]
AdjectivesChaotian /keɪˈoʊʃən/[3]
Symbol (astrological)
Orbital characteristics[4]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc5902 days (16.16 yr)
Earliest precovery date17 October 1991
Aphelion50.636 AU (7.5750 Tm)
Perihelion40.957 AU (6.1271 Tm)
Semi-major axis
45.796 AU (6.8510 Tm)
Eccentricity0.10567
Orbital period (sidereal)
309.92 yr (113199 d)
Average orbital speed
4.3931 km/s
Mean anomaly
337.2998°
Mean motion
0° 0m 11.449s / day
Inclination12.0502°
Longitude of ascending node
50.0239°
Time of perihelion
≈ 23 December 2033[5]
±10 days
Argument of perihelion
58.4097°
Jupiter MOID35.8 AU (5.36 Tm)
Neptune MOID12.5 AU (1.87 Tm)[6]
TJupiter5.884
Physical characteristics
Dimensions612 km (est. at 0.05)[7]
600+140
−130 km [8]
~665 [9]
Geometric albedo
0.050+0.030
−0.016 [8]
Spectral type
B–V=0.95±0.03 [9]
V–R=0.63±0.03 [9]
V–I=1.25±0.04 [9]
Absolute magnitude (H)
4.8 [4]
5.0 [7][9]
On 20 November 2020, Chaos occulted a magnitude 16.8 star. Three observers detected the occultation, finding that the object is likely smaller than 600 km in diameter. [10] Another occultation was recorded on 14 January 2022; full results on size, shape, geometric albedo, and the spin-axis orientation have not been released. [11] A further occultation occurred on 28 September 2023, with a shadow crossing most of North America. This occultation was observed by over 30 observers;[12] preliminary analysis suggests that Chaos is a binary (possibly a contact binary). [13]
Name
It is named after the primeval state of existence in Greek mythology, from which the first gods appeared.
Planetary symbols are no longer much used in astronomy, so Chaos never received a symbol in the astronomical literature. There is no standard symbol for Chaos used by astrologers either. Michael Moorcock's Symbol of Chaos () has been used. [14]
Orbit
19521 Chaos has an orbital period of approximately 309 years. Its orbit is longer, but less eccentric than the orbit of Pluto. 19521 Chaos's orbit is inclined approximately 12° to the ecliptic. Its orbit never crosses the orbit of Neptune. Currently, the closest approach possible to Neptune (MOID) is 12.5 AU (1.87 billion km). [6]
Chaos will come to perihelion at around December 2033,[5] coming as close as 40 AUs from Earth. Its brightest magnitude will be 20.8.
References
1. "MPEC 2008-O05 : Distant Minor Planets (2008 AUG. 2.0 TT)". Minor Planet Center. 17 July 2008. Retrieved 8 January 2011.
2. Buie, Marc W. (9 November 2004). "Orbit Fit and Astrometric record for 19521". Space Science Department. SwRI. Retrieved 28 September 2008.
3. Thayer (1994). Gray World, Green Heart. Wiley. ISBN 9780471572732.
4. "19521 Chaos (1998 WH24)". JPL Small-Body Database Browser (2007-12-14 last obs). Retrieved 11 April 2016.
5. JPL Horizons Observer Location: @sun (Perihelion occurs when deldot changes from negative to positive. Uncertainty in time of perihelion is 3-sigma.)
6. "(19521) Chaos = 1998 WH24 orbit". IAU Minor Planet Center. Retrieved 10 February 2018.
7. Brown, Michael E. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 25 December 2018.
8. Vilenius, E.; Kiss, C.; Mommert, M.; Müller, T.; Santos-Sanz, P.; Pal, A.; et al. (2012). ""TNOs are cool": A survey of the trans-Neptunian region VI. Herschel / PACS observations and thermal modeling of 19 classical Kuiper belt objects". Astronomy and Astrophysics. 541: A94. arXiv:1204.0697v1. Bibcode:2012A&A...541A..94V. doi:10.1051/0004-6361/201118743. S2CID 54222700.
9. Doressoundiram, A.; Peixinho, N.; de Bergh, C.; Fornasier, S.; Thébault, Ph. ; Barucci, M.A. ; Veillet, C. (October 2002). "The color distribution in the Edgeworth-Kuiper Belt". The Astronomical Journal. 124 (4): 2279–2296. arXiv:astro-ph/0206468. Bibcode:2002AJ....124.2279D. doi:10.1086/342447. S2CID 30565926.
10. Vara-Lubiano, Mónica; Morales, Nicolás; Rommel, Flavia; Ortiz, José Luis; Sicardy, Bruno; Santos-Sanz, Pablo; et al. (September 2021). The multi-chord stellar occultation by (19521) Chaos on 2020 November 20. 15th Europlanet Science Congress 2021. Europlanet Society. Bibcode:2021EPSC...15..626V. doi:10.5194/epsc2021-626. EPSC2021-626. Retrieved 26 June 2022.
11. Ortiz, José Luis; Morales, Nicolás; Vara-Lubiano, Mónica; Kretlow, Mike; Sicardy, Bruno; Santos-Sanz, Pablo; et al. (September 2022). The Trans-Neptunian Object (19521) Chaos as seen from stellar occultations and photometry observations. 16th Europlanet Science Congress 2022. Europlanet Society. doi:10.5194/epsc2022-520. EPSC2022-520. Retrieved 2 January 2023.
12. Gault, Dave. "OccultWatcher Cloud". OccultWatcher. Retrieved 29 September 2023.
13. Gómez-Limón Gallardo, José María; Leiva, R.; Ortiz, J. L.; Desmars, J.; Kilic, Y.; Vara-Lubiano, M.; Santos-Sanz, P.; Kretlow, M.; Rommel, F. L.; Morales, N.; Fernandez-Valenzuela, E.; Souami, D.; Lucky Star Team; Observers of Nov. 2020, Jan 2022, Dec 2022; Mar 2023 Occultations (2023). "Chaos: Stellar Occultations Reveal a Binary Tno?". Seventh Edition of the Spanish Meeting of Planetary Sciences and Exploration of the Solar System (7Th Cpess. Bibcode:2023pses.conf80462G. | 36 | 0 |
{{cite journal}}: CS1 maint: multiple names: authors list (link) CS1 maint: numeric names: authors list (link)
14. Miller, Kirk (26 October 2021). "Unicode request for dwarf-planet symbols" (PDF). unicode.org.
External links
• "Original Minor Planet Electronic Circular (1998-X08) for 19521 Chaos".
• "Revised Minor Planet Electronic Circular (1999-V03) 19521 Chaos".
• 19521 Chaos at AstDyS-2, Asteroids—Dynamic Site
• Ephemeris · Observation prediction · Orbital info · Proper elements · Observational info
• 19521 Chaos at the JPL Small-Body Database
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