Astronomy:(6265) 1985 TW3

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(6265) 1985 TW3
Discovery[1]
Discovered byT. F. Fric
R. J. Gilbrech
Discovery sitePalomar Obs.
Discovery date11 October 1985
Designations
(6265) 1985 TW3
1985 TW3 · 1953 RK1
1969 TZ4 · 1979 YG9
1985 VQ1 · 1987 GD1
1990 CX
Minor planet categorymain-belt[1][2] · (inner)
background[3]
Orbital characteristics[2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc48.42 yr (17,685 d)
|{{{apsis}}}|helion}}2.5839 AU
|{{{apsis}}}|helion}}1.7476 AU
2.1658 AU
Eccentricity0.1931
Orbital period3.19 yr (1,164 d)
Mean anomaly228.64°
Mean motion0° 18m 33.12s / day
Inclination4.1152°
Longitude of ascending node45.173°
281.59°
Known satellites1 (D: 1.16 km; P: 15.9 h)[4][5]
Physical characteristics
Mean diameter4.954±0.100 km[6][7][8]
5.20±0.22 km[9]
Rotation period2.70932±0.00008 h[10]
Geometric albedo0.285[9]
0.286[6]
0.2865[8]
L (SDSS-MOC)[11]
Absolute magnitude (H)13.40[9]
13.50[6][8]
13.6[1][2][12]


(6265) 1985 TW3 (provisional designation 1985 TW3) is a background asteroid and binary system from the inner regions of the asteroid belt. It was discovered on 11 October 1985, by astronomer by T. F. Fric and Richard Gilbrech at the Palomar Observatory in California. It is the only minor-planet discovery for these two astronomers.[1] The stony L-type asteroid measures approximately 5 kilometers (3.1 miles) in diameter and has a rotation period of 2.7 hours.[12] Its 1.2-kilometer sized minor-planet moon was discovered in July 2007 and announced the following month.[4]

Orbit and classification

1985 TW3 is a non-family asteroid from the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[3] Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[12]

It orbits the Sun in the inner asteroid belt at a distance of 1.7–2.6 AU once every 3 years and 2 months (1,164 days; semi-major axis of 2.17 AU). Its orbit has an eccentricity of 0.19 and an inclination of 4° with respect to the ecliptic.[2] It was first observed as 1953 RK1 at the former Alma-Ata Observatory (210) in September 1953. The body's observation arc begins with its observation as 1979 YG9 at Crimea–Nauchnij in December 1979, or almost 6 years prior to its official discovery observation at Palomar Observatory.[1]

Numbering and naming

This minor planet was permanently numbered (6265) by the Minor Planet Center on 17 March 1995 (M.P.C. 24890–24891).[13] As of 2018, it has not been named.[1]

Physical characteristics

In the SDSS-based taxonomy, 1985 TW3 is an unusual L-type asteroid.[11]

Rotation period

In June 2010, a rotational lightcurve of 1985 TW3 was obtained from photometric observations by Australian astronomers David Higgins and Julian Oey at the Hunters Hill (E14) and Leura Observatory (E17). Lightcurve analysis gave a well-defined rotation period of 2.70932±0.00008 hours with a brightness variation of 0.35 magnitude ({{{1}}}).[10] Several concurring period determinations in the range of 2.7091 to 2.710 hours with an amplitude of 0.26 to 0.36 magnitude were also made between 2007 and 2013 ({{{1}}}).[14][5][15][16][17]

Satellite

During a previous photometric observation by David Higgins on 15 July 2007, it was revealed that 1985 TW3 is a binary asteroid with a minor-planet moon in its orbit. The discovery was announced on 2 August 2007.[5] The satellite, provisional designation S/2007 (6265) 1, measures approximately 1.16 kilometers. It is separated by 8 km from its primary, orbiting it once every 15 hours and 52 minutes (15.859 hours or 0.6608 days).[4]

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), 1985 TW3 measures between 4.95 and 5.20 kilometers in diameter and its surface has an albedo between 0.285 and 0.287.[6][7][8][9] The Johnston's archive derives a diameter of 4.81 km and 1.16 km for the primary and secondary, respectively, based on an effective WISE-diameter of 4.95 km and using the lower limit of 0.24 for the secondary-to-primary diameter-ratio (Ds/p) determined by David Higgins.[4][5] Later observation by Higgins and Pravec determined a Ds/p ratio of 0.30 to 0.32,[10][15] which increases the satellites size by a quarter to a third if all other factors remain unchanged. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for members of the Flora family of 0.24 and calculates a diameter of 5.17 kilometers based on an absolute magnitude of 13.6.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "6265 (1985 TW3)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=6265. 
  2. ↑ 2.0 2.1 2.2 2.3 "JPL Small-Body Database Browser: 6265 (1985 TW3)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2006265. 
  3. ↑ 3.0 3.1 "Asteroid (6265) 1985 TW3". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=6265. 
  4. ↑ 4.0 4.1 4.2 4.3 Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database – (6265) 1985 TW3". Johnston's Archive. http://www.johnstonsarchive.net/astro/astmoons/am-06265.html. 
  5. ↑ 5.0 5.1 5.2 5.3 Higgins, D.; Pravec, P.; Kusnirak, P. (August 2007). "(6265) 1985 TW3". Central Bureau Electronic Telegrams 1015 (1015): 1. Bibcode: 2007CBET.1015....1H. http://www.cbat.eps.harvard.edu/iau/cbet/001000/CBET001015.txt. Retrieved 26 November 2018. 
  6. ↑ 6.0 6.1 6.2 6.3 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R. et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode: 2016PDSS..247.....M. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_COMPIL_5_NEOWISEDIAM_V1_0/data/neowise_mainbelt.tab. Retrieved 26 November 2018. 
  7. ↑ 7.0 7.1 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. doi:10.1088/0004-637X/741/2/68. Bibcode: 2011ApJ...741...68M. 
  8. ↑ 8.0 8.1 8.2 8.3 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.  (catalog)
  9. ↑ 9.0 9.1 9.2 9.3 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. 
  10. ↑ 10.0 10.1 10.2 Higgins, David; Oey, Julian; Pravec, Petr (January 2011). "Period Determination of Binary Asteroid Targets Observed at Hunters Hill Observatory: May-September 2009". The Minor Planet Bulletin 38 (1): 46–49. ISSN 1052-8091. Bibcode: 2011MPBu...38...46H. 
  11. ↑ 11.0 11.1 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. doi:10.1051/0004-6361/200913322. Bibcode: 2010A&A...510A..43C. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_I0035_5_SDSSTAX_V1_1/data/sdsstax_ast_table.tab. Retrieved 30 October 2019.  (PDS data set)
  12. ↑ 12.0 12.1 12.2 12.3 "LCDB Data for (6265)". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=6265%7C. 
  13. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 
  14. ↑ Bianchi, E. (December 1920). "Osservazioni fotometriche di pianeti". Memorie della Società Astronomia Italiana 2: 45. Bibcode: 1921MmSAI...2...45B. 
  15. ↑ 15.0 15.1 Pravec, P.; Scheirich, P.; Vokrouhlický, D.; Harris, A. W.; Kusnirák, P.; Hornoch, K. et al. (March 2012). "Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries". Icarus 218 (1): 125–143. doi:10.1016/j.icarus.2011.11.026. Bibcode: 2012Icar..218..125P. 
  16. ↑ Oey, Julian (October 2014). "Lightcurve Analysis of Asteroids from Blue Mountains Observatory in 2013". The Minor Planet Bulletin 41 (4): 276–281. ISSN 1052-8091. Bibcode: 2014MPBu...41..276O. 
  17. ↑ 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. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. 

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