4009 Drobyshevskij

4009 Drobyshevskij
Discovery [1]
Discovered byN. Chernykh
Discovery siteCrimea–Nauchnij
Discovery date13 March 1977
Designations
(4009) Drobyshevskij
Named after
Edward Drobyshevski [1]
(Russian astrophysicist)
1977 EN1 · 1982 BP3
1984 SP5
main-belt [1][2] · (outer)
Themis [3][4]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc53.96 yr (19,708 d)
Aphelion3.5557 AU
Perihelion2.7232 AU
3.1394 AU
Eccentricity0.1326
5.56 yr (2,032 d)
92.040°
0° 10m 37.92s / day
Inclination2.2916°
72.297°
181.12°
Physical characteristics
14.19 km (calculated)[3]
16.31±1.16 km[5]
18.198±0.236 km[6][7]
3.87±0.02 h[8]
3.875±0.0060 h (S)[9]
3.882±0.0060 h (R)[9]
0.044±0.008[6][7]
0.071±0.011[5]
0.08 (assumed)[3]
C [10] · C (assumed)[3]
12.4[7] · 12.50[5]
12.54±0.15 (R)[8]
12.577±0.003 (R)[9]
12.6[2][3] · 12.84[10]

4009 Drobyshevskij, provisional designation 1977 EN1, is a carbonaceous Themistian asteroid from the outer regions of the asteroid belt, approximately 16 kilometers (10 miles) in diameter. It was discovered on 13 March 1977, by Soviet–Russian astronomer Nikolai Chernykh at the Crimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula, and named after Russian astrophysicist Edward Drobyshevski.[1] The C-type asteroid has a relatively short rotation period of 3.875 hours.[3]

Orbit and classification

Drobyshevskij is a core member of the Themis family (602),[3][4] a very large family of carbonaceous asteroids, named after 24 Themis, the family's parent body.[11] It orbits the Sun in the outer main-belt at a distance of 2.7–3.6 AU once every 5 years and 7 months (2,032 days; semi-major axis of 3.14 AU). Its orbit has an eccentricity of 0.13 and an inclination of 2° with respect to the ecliptic.[2]

The body's observation arc begins with a precovery taken at the Goethe Link Observatory in November 1963, more than 13 years prior to its official discovery observation at Crimea–Nauchnij.[1]

Physical characteristics

Drobyshevskij has been characterized as a C-type asteroid by Pan-STARRS photometric survey. CALL also assumes it to be a carbonaceous C-type,[3] according to the Themistian asteroid's overall spectral type.[11]: 23 

Rotation period

Three rotational lightcurves of Drobyshevskij were obtained from photometric observations by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period between 3.87 and 3.882 hours with a brightness amplitude between 0.31 and 0.38 magnitude (U=2/2/2).[8][9] The Collaborative Asteroid Lightcurve Link (CALL) adopts a period of 3.875 hours from observations made in the S-band as the best result.[3] While not being a fast rotator, the body's period is relatively short.

Diameter and albedo

According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Drobyshevskij measures between 16.31 and 18.198 kilometers in diameter and its surface has an albedo between 0.044 and 0.071.[5][6][7] CALL assumes an albedo of 0.08 and calculates a diameter of 14.19 kilometers based on an absolute magnitude of 12.6.[3]

Naming

This minor planet was named after Edward Drobyshevski (1936–2012), who was a Russian astrophysicist at the Ioffe Institute of the Russian Academy of Sciences in Saint Petersburg, Russia. He is known for his cosmogonical models and theories about the origin of the small Solar System bodies as well as for his research on stellar magnetic fields. The official naming citation was published by the Minor Planet Center on 18 February 1992 (M.P.C. 19694).[12]

References

  1. ^ a b c d e "4009 Drobyshevskij (1977 EN1)". Minor Planet Center. Retrieved 18 March 2018.
  2. ^ a b c d "JPL Small-Body Database Browser: 4009 Drobyshevskij (1977 EN1)" (2017-10-27 last obs.). Jet Propulsion Laboratory. Retrieved 18 March 2018.
  3. ^ a b c d e f g h i j "LCDB Data for (4009) Drobyshevskij". Asteroid Lightcurve Database (LCDB). Retrieved 18 March 2018.
  4. ^ a b "Asteroid 4009 Drobyshevskij – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 27 October 2019.
  5. ^ 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. (online, AcuA catalog p. 153)
  6. ^ a b c 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. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68.
  7. ^ a b c d 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.
  8. ^ a b c Chang, Chan-Kao; Lin, Hsing-Wen; Ip, Wing-Huen; Prince, Thomas A.; Kulkarni, Shrinivas R.; Levitan, David; et al. (December 2016). "Large Super-fast Rotator Hunting Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series. 227 (2): 13. arXiv:1608.07910. Bibcode:2016ApJS..227...20C. doi:10.3847/0067-0049/227/2/20.
  9. ^ a b c d 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.
  10. ^ a b 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.
  11. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
  12. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 18 March 2018.