1035 Amata

1035 Amata
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 29 September 1924
Designations
MPC designation 1035 Amata
Named after
 Amata (Roman mythology)[2]
1924 SW · 1935 SU
1969 TJ4 · A913 UC
main-belt · (outer) [3]
Orbital characteristics [1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 102.55 yr (37,455 days)    
Aphelion 3.7603 AU
Perihelion 2.5485 AU
3.1544 AU
Eccentricity 0.1921
5.60 yr (2,046 days)
207.56°
0° 10m 33.24s / day
Inclination 18.043°
1.9593°
323.87°
Physical characteristics
Dimensions 50.69±2.9 km (IRAS:5)[4]
50.74 km (derived)[3]
59.28±0.79 km[5]
59.838±0.563 km[6]
60±6 km[7]
62.22±1.11 km[8]
9.05±0.01 h[9]
9.081±0.001 h[10]
9.7±0.07 h[11]
9.08215±0.00001 h[12]
0.0374±0.0079[6]
0.038±0.003[8]
0.039±0.001[5]
0.04±0.01[7]
0.0522±0.006 (IRAS:5)[4]
0.0571 (derived)[3]
C [3]
10.2[3][7][8]
10.3[1][4][5][6]

    1035 Amata, provisional designation 1924 SW, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 55 kilometers in diameter. It was discovered by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany on 29 September 1924.[13]

    The C-type asteroid orbits the Sun at a distance of 2.5–3.8 AU once every 5 years and 7 months (2,046 days). Its orbit has an eccentricity of 0.19 and an inclination of 18° with respect to the plane of the ecliptic.[1] The first used observation at the discovering observatory dates back to 1913, extending the asteroid's observation arc by 11 years prior to its discovery.[13]

    In October 2002, a rotational light-curve for this asteroid was obtained from photometric observations by American amateur astronomer Robert Stevens at the Santana Observatory (646) in California. It gave a rotation period of 9.081±0.001 hours with a brightness variation of 0.44 in magnitude (U=3).[10] In the same month, another observation was made at the Oakley Observatory in the U.S. state of Indiana and gave a very similar period of 9.05±0.01 hours and a variation in brightness of 0.32 in magnitude (U=2).[9]

    According to the space-based surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid has a low albedo between 0.038 and 0.052, and a diameter between 50.7 and 62.2 kilometers.[4][5][6][8][7] The Collaborative Asteroid Lightcurve Link derived a diameter of 50.7 kilometers and an albedo of 0.057.[3]

    The asteroid's name is of uncertain origin. It is thought to have been named after Amata, wife of King Latinus in Roman mythology and a character in Virgil's Aeneid. She is also the mother of Lavinia, the wife of Aeneas, after whom 1172 Äneas, one of the largest Jupiter trojans, is named.[2]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1035 Amata (1924 SW)" (2016-05-18 last obs.). Jet Propulsion Laboratory. Retrieved 7 June 2016.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1035) Amata. Springer Berlin Heidelberg. p. 89. ISBN 978-3-540-00238-3. Retrieved 7 June 2016.
    3. 1 2 3 4 5 6 "LCDB Data for (1035) Amata". Asteroid Lightcurve Database (LCDB). Retrieved 7 June 2016.
    4. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 7 June 2016.
    5. 1 2 3 4 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. Retrieved 7 June 2016.
    6. 1 2 3 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:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 7 June 2016.
    7. 1 2 3 4 Alí-Lagoa, V.; de León, J.; Licandro, J.; Delbó, M.; Campins, H.; Pinilla-Alonso, N.; et al. (June 2013). "Physical properties of B-type asteroids from WISE data". Astronomy and Astrophysics. 554: 16. arXiv:1303.5487Freely accessible. Bibcode:2013A&A...554A..71A. doi:10.1051/0004-6361/201220680. Retrieved 7 June 2016.
    8. 1 2 3 4 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:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 7 June 2016.
    9. 1 2 Kirkpatrick, Elaine; Hirsch, Brian; Lecrone, Crystal; Schwoenk, Dustin; Shiery, Michael; Tollefson, Eric; et al. (September 2003). "Oakley Observatory lightcurves of asteroids 670 Ottegebe and 1035 Amata". The Minor Planet Bulletin. 30 (3): 41. Bibcode:2003MPBu...30...41K. ISSN 1052-8091. Retrieved 7 June 2016.
    10. 1 2 Stephens, Robert D. (December 2002). "Photometry of 1035 Amata and 1829 Dawson". The Minor Planet Bulletin. 30 (2): 31. Bibcode:2003MPBu...30...31S. ISSN 1052-8091. Retrieved 7 June 2016.
    11. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (1035) Amata". Geneva Observatory. Retrieved 7 June 2016.
    12. ↑ Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv:1601.02909Freely accessible. Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. Retrieved 7 June 2016.
    13. 1 2 "1035 Amata (1924 SW)". Minor Planet Center. Retrieved 7 June 2016.

    External links

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