3640 Gostin

3640 Gostin
Discovery [1]
Discovered by C. Shoemaker
E. Shoemaker
Discovery site Palomar Obs.
Discovery date 11 October 1985
Designations
MPC designation (3640) Gostin
Named after
 Victor Gostin [1]
(Australian geologist)
1985 TR3 · 1955 SS
1960 CB · 1970 CS
1972 VJ1
main-belt [1][2] · (inner)
Flora [3][4]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 61.63 yr (22,511 d)
Aphelion 2.4175 AU
Perihelion 2.0311 AU
2.2243 AU
Eccentricity 0.0869
3.32 yr (1,212 d)
224.62°
0° 17m 49.56s / day
Inclination 4.3118°
289.19°
155.59°
Physical characteristics
Mean diameter
 7.148±0.088 km[5]
7.613±0.096 km[6]
8.58 km (calculated)[3]
3.26±0.05 h[7]
3.263±0.0009 h[8]
3.263±0.003 h[9]
3.2641±0.0005 h[10]
0.2127±0.0446[6]
0.239±0.036[5]
0.24 (assumed)[3]
SMASS = S [2][3]
12.26±0.14 (R)[7]
12.398±0.001 (R)[8]
12.5[2][3]
12.62±0.20[11]
12.9[6]

    3640 Gostin, provisional designation 1985 TR3, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 8 kilometers (5 miles) in diameter. It was discovered on 11 October 1985, by American astronomer couple Carolyn and Eugene Shoemaker at the Palomar Observatory in California.[1] The S-type asteroid has a rotation period of 3.26 hours.[3] It was named for Australian geologist Victor Gostin.[1]

    Orbit and classification

    Gostin is a member of the Gondolatsch-cluster within the Flora family (402),[3][4] a giant asteroid family and the largest family of stony asteroids in the main-belt,[12]

    It orbits the Sun in the inner main-belt at a distance of 2.0–2.4 AU once every 3 years and 4 months (1,212 days; semi-major axis of 2.22 AU). Its orbit has an eccentricity of 0.09 and an inclination of 4° with respect to the ecliptic.[2] The body's observation arc begins with its first observation as 1955 SS at the Goethe Link Observatory in September 1955, or 30 years prior to its official discovery observation at Palomar.[1]

    Physical characteristics

    In the SMASS classification, Gostin is a common, stony S-type asteroid.[2]

    Rotation period

    In March 2010, a rotational lightcurve of Gostin was obtained from photometric observations at the Oakley Southern Sky Observatory. Lightcurve analysis gave a well-defined rotation period of 3.2641 hours with a brightness variation of 0.40 magnitude (U=3).[10] Concurring lightcurves were also obtained at the Palomar Transient Factory and at the Etscorn Campus Observatory (U=3/2/3).[3][7][8][9]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Gostin measures 7.148 and 7.613 kilometers in diameter and its surface has an albedo of 0.239 and 0.2127, respectively.[5][6] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from 8 Flora, the parent body of the Flora family – and calculates a diameter of 8.58 kilometers based on an absolute magnitude of 12.5.[3]

    Naming

    This minor planet was named by the discoverers after Australian geologist Victor Gostin (born 1940) of the University of Adelaide, who in the 1980s discovered the ejecta layer from the Acraman bolide impact at a distance of 300 kilometers from the impact site, within Ediacaran sedimentary rocks of the Flinders Ranges, South Australia, which enabled the impact to be dated at ~580 Ma.[1][13] The official naming citation was published by the Minor Planet Center on 2 February 1988 (M.P.C. 12808).[14]

    References

    1. 1 2 3 4 5 6 7 "3640 Gostin (1985 TR3)". Minor Planet Center. Retrieved 15 May 2018.
    2. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 3640 Gostin (1985 TR3)" (2017-05-05 last obs.). Jet Propulsion Laboratory. Retrieved 15 May 2018.
    3. 1 2 3 4 5 6 7 8 9 "LCDB Data for (3640) Gostin". Asteroid Lightcurve Database (LCDB). Retrieved 15 May 2018.
    4. 1 2 "Asteroid 3669 Vertinskij". Small Bodies Data Ferret. Retrieved 15 May 2018.
    5. 1 2 3 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" (PDF). The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 15 May 2018.
    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" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 15 May 2018. (catalog)
    7. 1 2 3 Chang, Chan-Kao; Ip, Wing-Huen; Lin, Hsing-Wen; Cheng, Yu-Chi; Ngeow, Chow-Choong; Yang, Ting-Chang; et al. (June 2014). "313 New Asteroid Rotation Periods from Palomar Transient Factory Observations". The Astrophysical Journal. 788 (1): 21. arXiv:1405.1144. Bibcode:2014ApJ...788...17C. doi:10.1088/0004-637X/788/1/17. Retrieved 15 May 2018.
    8. 1 2 3 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" (PDF). The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 15 May 2018.
    9. 1 2 Klinglesmith, Daniel A., III; Hendrickx, Sebastian; Madden, Karl; Montgomery, Samuel (April 2016). "Lightcurves for Shape/Spin Models". The Minor Planet Bulletin. 43 (2): 123–128. Bibcode:2016MPBu...43..123K. ISSN 1052-8091. Retrieved 15 May 2018.
    10. 1 2 Albers, Kenda; Kragh, Katherine; Monnier, Adam; Pligge, Zachary; Stolze, Kellen; West, Josh; et al. (October 2010). "Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2009 October thru 2010 April". The Minor Planet Bulletin. 37 (4): 152–158. Bibcode:2010MPBu...37..152A. ISSN 1052-8091. Retrieved 15 May 2018.
    11. ↑ 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" (PDF). Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 15 May 2018.
    12. ↑ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 15 May 2018.
    13. ↑ Gostin, V. A.; Haines, P. W.; Jenkins, R. J. F.; Compston, W.; Williams, I. S. (July 1986). "Impact ejecta horizon within late Precambrian shales, Adelaide Geosyncline, South Australia". Science: 198–200. Bibcode:1986Sci...233..198G. doi:10.1126/science.233.4760.198. ISSN 0036-8075. Retrieved 15 May 2018.
    14. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 15 May 2018.

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