4786 Tatianina

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4786 Tatianina
Discovery [1]
Discovered byN. Chernykh
Discovery siteCrimean Astrophysical Obs.
Discovery date13 August 1985
Designations
MPC designation(4786) Tatianina
Named after
Tatiana Somova [1]
(Friend of discoverer)
1985 PE2 · 1948 GA
1970 KF · 1984 EV1
1984 FM1
main-belt[1][2] · (inner)[3]
background[4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc47.10 yr (17,202 d)
Aphelion2.8145 AU
Perihelion1.9011 AU
2.3578 AU
Eccentricity0.1937
3.62 yr (1,322 d)
83.900°
0° 16m 19.92s / day
Inclination7.2560°
115.77°
118.27°
Known satellites1 (D: 0.61 km P: 21.67 h)[3][5][6][a]
Physical characteristics
Mean diameter
3.282±0.197 km[7][8]
3.475 km[9]
3.48 km (taken)[3]
2.9227±0.0001 h[a]
2.9227 h[6]
2.9228±0.0003 h[10]
0.4763[9]
0.5136±0.1593[8]
0.514±0.159[7]
SMASS = Xc[2] · E[8]
13.3[2]
13.31±0.1 (R)[a]
13.46±0.20[11]
13.718±0.1[3][9]
13.76[8]

4786 Tatianina, provisional designation 1985 PE2, is a bright background asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 3.4 kilometers (2.1 miles) in diameter. It was discovered on 13 August 1985, by Soviet astronomer Nikolai Chernykh at the Crimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula.[1] It was named after Tatiana Somova, a friend of the discoverer. The E-/Xc-subtype has a short rotation period of 2.9 hours.[3] Its sub-kilometer minor-planet moon was discovered on 20 March 2006 and announced the following month.[5][6]

Orbit and classification[edit]

Tatianina is a non-family asteroid from the main belt's background population.[4] It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.8 AU once every 3 years and 7 months (1,322 days; semi-major axis of 2.36 AU). Its orbit has an eccentricity of 0.19 and an inclination of 7° with respect to the ecliptic.[2]

The asteroid was first observed as 1948 GA at the Algiers Observatory in April 1948. The body's observation arc begins at Nauchnij in May 1970 as 1970 KF, more than 15 years prior to its official discovery observation.[1]

Physical characteristics[edit]

In the SMASS classification, Tatianina is a Xc-subtype that transitions from the X-type to the carbonaceous C-type asteroids.[2] It has also been characterized as a bright E-type by the Wide-field Infrared Survey Explorer (WISE).[3][8]

Rotation period[edit]

Several rotational lightcurves of Tatianina have been obtained from photometric observations since 2003 (U=3/2+/3).[6][10][a] Analysis of the best-rated lightcurve from March 2003, during which a satellite was also discovered (see below), gave a rotation period of 2.9227 hours with a brightness amplitude of 0.19 and 0.20 magnitude (U=3/3).[3][6][a]

Diameter and albedo[edit]

According to the survey carried out by the NEOWISE mission of NASA's WISE telescope, Tatianina measures between 3.282 and 3.475 kilometers in diameter and its surface has an exceptionally high albedo of 0.4763 to 0.514.[7][8][9] The Collaborative Asteroid Lightcurve Link adopts the revised WISE-data by Petr Pravec, that is an albedo of 0.4763 and rounded diameter of 3.48 kilometers based on an absolute magnitude of 13.718.[3]

Satellite[edit]

During the photometric observations by Donald Pray, Petr Pravec and collaborators in March 2006, it was revealed that Tatianina is a synchronous binary asteroid with a minor-planet moon orbiting it every 21.67 hours at an estimated average distance of 6.6 km. The discovery was announced on 11 April 2006.[6] The mutual occultation events suggest the presence of a satellite with an estimated diameter of 610±10 meters or 19% the size of its primary.[3][5][a]

Numbering and naming[edit]

This minor planet was numbered on 28 April 1991.[5] It was named by the discoverer after Tatiana Aleksandrovna Somova, a nursery-school teacher in Saint Petersburg, Russia.[1] The official naming citation was published by the Minor Planet Center on 5 March 1996 (M.P.C. 26762).[12]

Notes[edit]

  1. ^ a b c d e f (Pravec 2006) Lightcurve plots of (4786) Tatianina: Combined, Secondary and Primary. Rotation period in the R-band of 2.9227±0.0001 hours with a brightness amplitude of 0.19±0.02 mag. Quality code of 3. Binary detected. Summary figures at the LCDB and Pravec, P.; Wolf, M.; Sarounova, L. (2006). Plots from Ondrejov data obtained by the NEO Photometric Program and collaborating projects

References[edit]

  1. ^ a b c d e f "4786 Tatianina (1985 PE2)". Minor Planet Center. Retrieved 4 May 2018.
  2. ^ a b c d e f "JPL Small-Body Database Browser: 4786 Tatianina (1985 PE2)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 4 May 2018.
  3. ^ a b c d e f g h i "LCDB Data for (4786) Tatianina". Asteroid Lightcurve Database (LCDB). Retrieved 4 May 2018.
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 4 May 2018.
  5. ^ a b c d Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database – (4786) Tatianina". Johnston's Archive. Retrieved 4 May 2018.
  6. ^ a b c d e f Pray, D.; Pravec, P.; Kusnirak, P.; Nudds, S.; Galad, A.; Gajdos, S.; et al. (April 2006). "CBET 472 – (4786) Tatianina". Central Bureau Electronic Telegrams (472). Bibcode:2006CBET..472....1P. Retrieved 4 May 2018.
  7. ^ 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. Retrieved 4 May 2018.
  8. ^ a b c d e f 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 4 May 2018. (catalog)
  9. ^ a b c d Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 4 May 2018.
  10. ^ a b 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. Bibcode:2011MPBu...38...41H. ISSN 1052-8091. Retrieved 4 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 4 May 2018.
  12. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 May 2018.

External links[edit]