1035 Amata

From Wikipedia, the free encyclopedia

1035 Amata
001035-asteroid shape model (1035) Amata.png
Modelled shape of Amata from its lightcurve
Discovery[1]
Discovered byK. Reinmuth
Discovery siteHeidelberg Obs.
Discovery date29 September 1924
Designations
MPC designation
(1035) Amata
Pronunciation/əˈmeɪtə/[4]
Named after
Amata (Roman mythology)[2]
1924 SW · 1935 SU
1969 TJ4 · A913 UC
Minor planet category
main-belt · (outer)[3]
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc102.63 yr (37,484 days)
Aphelion3.7582 AU
Perihelion2.5551 AU
3.1566 AU
Eccentricity0.1906
5.61 yr (2,049 days)
242.46°
0° 10m 32.52s / day
Inclination18.030°
1.9593°
323.98°
Physical characteristics
Dimensions50.69±2.9 km (IRAS:5)[5]
50.74 km (derived)[3]
56.063±0.404[6]
59.28±0.79 km[7]
59.838±0.563 km[8]
60±6 km[9]
62.22±1.11 km[10]
Synodic rotation period
9.05±0.01 h[11]
9.081±0.001 h[12]
9.08215±0.00001 h[13]
9.7±0.07 h[14]
0.0374±0.0079[8]
0.038±0.003[10][6]
0.039±0.001[7]
0.04±0.01[9]
0.0522±0.006 (IRAS:5)[5]
0.0571 (derived)[3]
C[3]
Absolute magnitude (H)
10.2[3][9][10] · 10.3[1][5][7][8]

1035 Amata /əˈmeɪtə/ is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 57 kilometers in diameter. It was discovered by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany on 29 September 1924 and assigned the provisional designation 1924 SW.[15] It was probably named after Amata from Roman mythology.[2]

Classification and orbit[]

The C-type asteroid orbits the Sun at a distance of 2.6–3.8 AU once every 5 years and 7 months (2,049 days). Its orbit has an eccentricity of 0.19 and an inclination of 18° with respect to the ecliptic.[1] The first used observation was taken at the discovering observatory in 1913, extending the body's observation arc by 11 years prior to its discovery.[15]

Naming[]

Amata'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]

Unknown meaning[]

Among the many thousands of named minor planets, Amata is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between 164 Eva and 1514 Ricouxa and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth (also see category).[16]

Physical characteristics[]

In October 2002, a rotational light-curve of Amata 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).[12] 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).[11]

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, Amata measures between 50.7 and 62.2 kilometers in diameter, and its surface has a low albedo between 0.038 and 0.052.[5][6][7][8][9][10] The Collaborative Asteroid Lightcurve Link derived a diameter of 50.7 kilometers and an albedo of 0.057.[3]

References[]

  1. ^ a b c d "JPL Small-Body Database Browser: 1035 Amata (1924 SW)" (2016-06-16 last obs.). Jet Propulsion Laboratory. Retrieved 9 December 2016.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1035) Amata". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 89. doi:10.1007/978-3-540-29925-7_1036. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f "LCDB Data for (1035) Amata". Asteroid Lightcurve Database (LCDB). Retrieved 7 June 2016.
  4. ^ Noah Webster (1884) A Practical Dictionary of the English Language
  5. ^ a b c d 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 22 October 2019.
  6. ^ a b c 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. Retrieved 9 December 2016.
  7. ^ a b c d 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)
  8. ^ a b c d 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 7 June 2016.
  9. ^ a b c d 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:1303.5487. Bibcode:2013A&A...554A..71A. doi:10.1051/0004-6361/201220680. Retrieved 7 June 2016.
  10. ^ a b c d 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 7 June 2016.
  11. ^ a b 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.
  12. ^ a b 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.
  13. ^ Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv:1601.02909. Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. Retrieved 7 June 2016.
  14. ^ Behrend, Raoul. "Asteroids and comets rotation curves – (1035) Amata". Geneva Observatory. Retrieved 7 June 2016.
  15. ^ a b "1035 Amata (1924 SW)". Minor Planet Center. Retrieved 7 June 2016.
  16. ^ Schmadel, Lutz D. (2007). "Appendix 11 – Minor Planet Names with Unknown Meaning". Dictionary of Minor Planet Names – Fifth Revised and Enlarged revision. Springer Berlin Heidelberg. pp. 927–929. ISBN 978-3-540-00238-3.

External links[]

Retrieved from ""