1737 Severny
Discovery[1]
Discovered byL. Chernykh
Discovery siteCrimean Astrophysical Obs.
Discovery date13 October 1966
Designations
(1737) Severny
Named after
Andrei Severny
(observatory's director)[2]
1966 TJ · 1942 CA
1944 OF · 1950 TM
1950 TP4 · 1951 YF2
1963 DH
main-belt · Eos[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc65.83 yr (24,044 days)
Aphelion3.1578 AU
Perihelion2.8644 AU
3.0111 AU
Eccentricity0.0487
5.23 yr (1,908 days)
112.51°
Inclination9.3772°
327.44°
221.77°
Physical characteristics
Dimensions21.334±0.158[4]
21.40 km (calculated)[3]
21.61±2.7 km[5]
22.793±0.122 km[6]
24.83±1.47 km[7]
9.2481±0.0625 h[8]
14.11±0.07 h[9]
0.1363±0.0267[6]
0.139±0.018[7]
0.14 (assumed)[3]
0.175±0.031[4]
0.1811±0.057[5]
S[3]
10.67±0.58[10] · 10.8[5][7] · 11.0[6] · 11.018±0.002 (R)[8] · 11.1[1][3]

    1737 Severny, provisional designation 1966 TJ, is a stony Eoan asteroid from the outer region of the asteroid belt, approximately 21 kilometers in diameter.

    It was discovered on 13 October 1966, by Russian astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory in Nauchnyj, on the Crimean peninsula, who named after Soviet astronomer Andrei Severny.[2][11]

    Classification and orbit

    Severny is a member of the Eos family. It orbits the Sun in the outer main-belt at a distance of 2.9–3.2 AU once every 5 years and 3 months (1,908 days). Its orbit has an eccentricity of 0.05 and an inclination of 9° with respect to the ecliptic.[1] First identified as 1942 CA at Turku, the asteroid's first used observation was made at Heidelberg Observatory in 1950, extending Severny's observation arc by 16 years prior to its official discovery observation.[11]

    Physical characteristics

    Severny has been characterized as a common stony S-type asteroid.[3]

    Lightcurves

    A rotational lightcurve of Severny was obtained by French amateur astronomer Laurent Bernasconi in March 2005. It gave a rotation period of 14.11 hours with a brightness variation of 0.14 magnitude (U=2).[9]

    In September 2013, photometric observations in the R-band at the Palomar Transient Factory, California, gave a shorter period of 9.2481 hours with an amplitude of 0.17 magnitude (U=2).[8]

    Diameter and albedo

    According to the 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, Severny measures between 21.33 and 24.83 kilometers in diameter, and its surface has an albedo between 0.136 and 0.181.[4][5][6][7]

    The Collaborative Asteroid Lightcurve Link assumes a standard albedo for Eoan asteroids of 0.14 and calculates a diameter of 21.40 kilometers with an absolute magnitude of 11.1.[3]

    Naming

    This minor planet was named by the discoverer in honor of Soviet astronomer Andrei Severny (1913–1987), who was the Director of the Crimean Astrophysical Observatory[2] and known for his work on solar flares and astronomical observations from artificial satellites. The official naming citation was published by the Minor Planet Center on 1 October 1969 (M.P.C. 2971).[12]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1737 Severny (1966 TJ)" (2016-08-03 last obs.). Jet Propulsion Laboratory. Archived from the original on 18 September 2020. Retrieved 7 June 2017.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1737) Severny". Dictionary of Minor Planet Names – (1737) Severny. Springer Berlin Heidelberg. p. 138. doi:10.1007/978-3-540-29925-7_1738. ISBN 978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 "LCDB Data for (1737) Severny". Asteroid Lightcurve Database (LCDB). Retrieved 21 December 2016.
    4. 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". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 21 December 2016.
    5. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System – IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 17 October 2019.
    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". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    7. 1 2 3 4 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. 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". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 21 December 2016.
    9. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1737) Severny". Geneva Observatory. Retrieved 21 December 2016.
    10. ↑ 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:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 21 December 2016.
    11. 1 2 "1737 Severny (1966 TJ)". Minor Planet Center. Retrieved 21 December 2016.
    12. ↑ 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.
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