Astronomy:1619 Ueta

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1619 Ueta
001619-asteroid shape model (1619) Ueta.png
Shape model of Ueta from its lightcurve
Discovery[1]
Discovered byT. Mitani
Discovery siteKwasan Obs. (377)
Discovery date11 October 1953
Designations
(1619) Ueta
Named afterMr Ueta
(observatory's director)[2]
1953 TA · 1926 RR
1931 AO · 1940 YJ
1951 AG1 · 1978 GM
Minor planet categorymain-belt · (inner)[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc85.68 yr (31,293 days)
|{{{apsis}}}|helion}}2.6368 AU
|{{{apsis}}}|helion}}1.8454 AU
2.2411 AU
Eccentricity0.1766
Orbital period3.35 yr (1,225 days)
Mean anomaly5.9446°
Mean motion0° 17m 37.68s / day
Inclination6.2142°
Longitude of ascending node61.494°
328.18°
Physical characteristics
Dimensions7.13±0.40 km[4]
8.965±0.124 km[5]
9.927±0.066 km[6]
11.04 km (calculated)[3]
Rotation period2.717943±0.000005 h[7]
2.7180±0.0005 h[8]
2.718238±0.000001 h[9]
2.720±0.002 h[10]
2.720±0.005 h[11]
2.94 h (dated)[12]
Geometric albedo0.20 (assumed)[3]
0.2517±0.0317[6]
0.479±0.056[4]
Tholen = S[1] · S[3][13]
B–V = 0.900[1]
U–B = 0.546[1]
Absolute magnitude (H)12.48±0.28[13] · 12.15[1][3][4][6]


1619 Ueta, provisional designation 1953 TA, is a stony asteroid from the inner regions of the asteroid belt, approximately 11 kilometers in diameter. It was discovered on 11 October 1953, by Japanese astronomer Tetsuyasu Mitani at Kyoto University's Kwasan Observatory (377), near Kyoto, Japan.[14] It was named after the former director of the discovering observatory.[2]

Classification and orbit

Ueta is a S-type asteroid, that orbits the Sun in the inner main-belt at a distance of 1.8–2.6 AU once every 3 years and 4 months (1,225 days). Its orbit has an eccentricity of 0.18 and an inclination of 6° with respect to the ecliptic.[1]

It was first identified as 1926 RR at Johannesburg in 1926. Ueta's observation arc begins 22 years prior to its official discovery observation with a precovery taken at Lowell Observatory in 1931.[14]

Rotation period and pole

Several rotational lightcurves of Ueta were obtained from photometric observations. Best rated lightcurves were obtained by astronomers Robert Stephens and David Higgins in September 2009, securing an identical rotation period of 2.720 hours with a brightness variation of 0.35 and 0.39 magnitude, respectively ({{{1}}}).[10][11] Modeled lightcurves from various photometric data sources also gave a similar period of 2.717943 and 2.718238 hours ({{{1}}}).[7][9]

Diameter and albedo

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Ueta measures between 7.13 and 9.93 kilometers in diameter, and its surface has an albedo between 0.251 and 0.479.[4][5][6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 11.04 kilometers with an absolute magnitude of 12.15.[3]

Naming

Ueta was named by the discoverer for the former Director of Kwasan Observatory (also see § External links) who encouraged him to keep on with his observations of minor planets and comets.[2] The official naming citation was published by the Minor Planet Center on 1 February 1965 (M.P.C. 2347).[15]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "JPL Small-Body Database Browser: 1619 Ueta (1953 TA)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001619. Retrieved 30 June 2017. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(1619) Ueta". Dictionary of Minor Planet Names – (1619) Ueta. Springer Berlin Heidelberg. p. 128. doi:10.1007/978-3-540-29925-7_1620. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 "LCDB Data for (1619) Ueta". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1619%7CUeta. Retrieved 28 December 2016. 
  4. ↑ 4.0 4.1 4.2 4.3 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. doi:10.1088/2041-8205/759/1/L8. Bibcode: 2012ApJ...759L...8M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012ApJ...759L...8M. Retrieved 28 December 2016. 
  5. ↑ 5.0 5.1 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. doi:10.1088/0004-637X/791/2/121. Bibcode: 2014ApJ...791..121M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2014ApJ...791..121M. Retrieved 28 December 2016. 
  6. ↑ 6.0 6.1 6.2 6.3 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. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M. 
  7. ↑ 7.0 7.1 Hanus, J.; Broz, M.; Durech, J.; Warner, B. D.; Brinsfield, J.; Durkee, R. et al. (November 2013). "An anisotropic distribution of spin vectors in asteroid families". Astronomy and Astrophysics 559: 19. doi:10.1051/0004-6361/201321993. Bibcode: 2013A&A...559A.134H. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2013A&A...559A.134H. Retrieved 28 December 2016. 
  8. ↑ Kryszczynska, A.; Colas, F.; Polinska, M.; Hirsch, R.; Ivanova, V.; Apostolovska, G. et al. (October 2012). "Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region". Astronomy and Astrophysics 546: 51. doi:10.1051/0004-6361/201219199. Bibcode: 2012A&A...546A..72K. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012A&A...546A..72K. Retrieved 28 December 2016. 
  9. ↑ 9.0 9.1 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics 587: 6. doi:10.1051/0004-6361/201527573. Bibcode: 2016A&A...587A..48D. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2016A&A...587A..48D. Retrieved 28 December 2016. 
  10. ↑ 10.0 10.1 Higgins, David (January 2011). "Period Determination of Asteroid Targets Observed at Hunters Hill Observatory: May 2009 - September 2010". The Minor Planet Bulletin 38 (1): 41–46. ISSN 1052-8091. Bibcode: 2011MPBu...38...41H. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2011MPBu...38...41H. Retrieved 28 December 2016. 
  11. ↑ 11.0 11.1 Stephens, Robert D. (January 2011). "Asteroids Observed from GMARS and Santana Observatories: 2010 July - September". The Minor Planet Bulletin 38 (1): 23–24. ISSN 1052-8091. Bibcode: 2011MPBu...38...23S. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2011MPBu...38...23S. Retrieved 28 December 2016. 
  12. ↑ Almeida, R.; Angeli, C. A.; Duffard, R.; Lazzaro, D. (February 2004). "Rotation periods for small main-belt asteroids". Astronomy and Astrophysics 415: 403–406. doi:10.1051/0004-6361:20034585. Bibcode: 2004A&A...415..403A. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2004A&A...415..403A. Retrieved 28 December 2016. 
  13. ↑ 13.0 13.1 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 28 December 2016. 
  14. ↑ 14.0 14.1 "1619 Ueta (1953 TA)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1619. Retrieved 28 December 2016. 
  15. ↑ 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



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