1436 Salonta

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1436 Salonta
1436Salonta (Lightcurve Inversion).png
Lightcurve-based 3D-model of Salonta
Discovery [1]
Discovered by G. Kulin
Discovery site Konkoly Obs.
Discovery date 11 December 1936
Designations
MPC designation (1436) Salonta
Named after
Salonta[2] (Romanian city)
1936 YA · 1933 FX1
1934 NU · 1954 CQ
main-belt · (outer)[3]
background [4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 84.20 yr (30,754 days)
Aphelion 3.3424 AU
Perihelion 2.9502 AU
3.1463 AU
Eccentricity 0.0623
5.58 yr (2,038 days)
328.13°
0° 10m 35.76s / day
Inclination 13.889°
260.42°
29.895°
Physical characteristics
Dimensions 52.73±17.17 km[5]
53.769±0.269 km[6]
60.95±0.91 km[7]
62.90±1.6 km[8]
62.927±0.418 km[9]
65.53±15.83 km[10]
72.06±0.75 km[11]
8.861±0.003 h[12]
8.870±0.004 h[13][a]
8.8716±0.0007 h[12]
0.028±0.005[11][11]
0.03±0.02[10]
0.0338±0.0052[9]
0.0339±0.002[8]
0.037±0.001[7]
0.05±0.04[5]
P[9] · C (assumed)[3]
10.20[11][10] · 10.27±0.34[14] · 10.30[1][3][7][8][9] · 10.43[5]

1436 Salonta, provisional designation 1936 YA, is a dark background asteroid from the outer regions of the asteroid belt, approximately 60 kilometers in diameter. Discovered by György Kulin at the Konkoly Observatory in 1936, the asteroid was later named for the Romanian city of Salonta, the birthplace of the discoverer.

Discovery[edit]

Salonta was discovered on 11 December 1936, by Hungarian astronomer György Kulin at the Konkoly Observatory in Budapest.[15] Three nights later, it was independently discovered by French astronomer André Patry at Nice Observatory on 14 December 1936,[2] the Minor Planet Center only recognizes the first discoverer.[15] The asteroid was first identified as 1933 FX1 at Johannesburg Observatory in March 1933.[15]

Orbit and classification[edit]

Salonta is a non-family asteroid from the main belt's background population.[4] It orbits the Sun in the outer asteroid belt at a distance of 3.0–3.3 AU once every 5 years and 7 months (2,038 days). Its orbit has an eccentricity of 0.06 and an inclination of 14° with respect to the ecliptic.[1] The body's observation arc begins at the discovering Konkloy Observatory in January 1937, about one month after its official discovery observation.[15]

Physical characteristics[edit]

Salonta has been characterized as a dark and primitive P-type asteroid by the Wide-field Infrared Survey Explorer (WISE).[9] It is also an assumed carbonaceous C-type asteroid.[3]

Rotation period[edit]

In 2007 and 2008, three rotational lightcurves of Salonta were independently obtained from photometric observations by astronomers Brian Warner, Pierre Antonini and René Roy. Lightcurve analysis gave a well defined rotation period between 8.861 and 8.8716 hours with a brightness amplitude of 0.17 to 0.33 magnitude (U=3/3/3).[12][13][a]

Spin axis[edit]

In 2016, a lightcurve of Salonta has also been modeled using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and from individual observers. Modelling gave a concurring sidereal period of 8.86985 hours as well as two spin axis of (223.0°, 18.0°) and (57.0°, 35°) in ecliptic coordinates (λ, β).[16]

Diameter and albedo[edit]

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's WISE telescope, Salonta measures between 52.73 and 72.06 kilometers in diameter and its surface has an albedo between 0.028 and 0.05.[5][6][7][8][9][10][11]

The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0339 and a diameter of 62.90 kilometers based on an absolute magnitude of 10.3.[3]

Naming[edit]

This minor planet was named after the Romanian city of Salonta, formerly known as "Nagyszalonta" when it was still part of the Kingdom of Hungary, it is the birthplace of the discoverer György Kulin.[2] The official naming citation was published by the Minor Planet Center on 1 February 1980 (M.P.C. 5182).[17]

Notes[edit]

  1. ^ a b Lightcurve plot of 1436 Salonta, Palmer Divide Observatory, Brian D. Warner (2007). Summary figures at LCDB

References[edit]

  1. ^ a b c d "JPL Small-Body Database Browser: 1436 Salonta (1936 YA)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Retrieved 24 October 2017. 
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1436) Salonta. Springer Berlin Heidelberg. p. 115. ISBN 978-3-540-00238-3. Retrieved 24 October 2017. 
  3. ^ a b c d e "LCDB Data for (1436) Salonta". Asteroid Lightcurve Database (LCDB). Retrieved 24 October 2017. 
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 24 October 2017. 
  5. ^ a b c d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923Freely accessible. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 24 October 2017. 
  6. ^ a b 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:1406.6645Freely accessible. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 24 October 2017. 
  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. Retrieved 24 October 2017. 
  8. ^ 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. Bibcode:2004PDSS...12.....T. Retrieved 24 October 2017. 
  9. ^ a b c d e f Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 24 October 2017. 
  10. ^ a b c d 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:1509.02522Freely accessible. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 24 October 2017. 
  11. ^ a b c d e 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 24 October 2017. 
  12. ^ a b c Behrend, Raoul. "Asteroids and comets rotation curves – (1436) Salonta". Geneva Observatory. Retrieved 24 October 2017. 
  13. ^ a b Warner, Brian D. (June 2008). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory - June - October 2007". The Minor Planet Bulletin. 35 (2): 56–60. Bibcode:2008MPBu...35...56W. ISSN 1052-8091. Retrieved 24 October 2017. 
  14. ^ 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:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 24 October 2017. 
  15. ^ a b c d "1436 Salonta (1936 YA)". Minor Planet Center. Retrieved 24 October 2017. 
  16. ^ Hanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution" (PDF). Astronomy and Astrophysics. 551: 16. arXiv:1301.6943Freely accessible. Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. Retrieved 24 October 2017. 
  17. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 October 2017. 

External links[edit]