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3322 Lidiya

From Wikipedia, the free encyclopedia
Phocaea asteroid and potentially slow rotator

3322 Lidiya
Discovery[1]
Discovered byT. Smirnova
Discovery siteCrimean Astrophysical Obs.
Discovery date1 December 1975
Designations
(3322) Lidiya
Named after
Lidiya Zvereva
(Russian aviator)[2]
1975 XY1 · 1975 VJ6
main-belt · (inner)
Phocaea[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc41.49 yr (15,153 days)
Aphelion2.9105AU
Perihelion1.8738 AU
2.3921 AU
Eccentricity0.2167
3.70yr (1,351 days)
72.866°
0° 15m 59.04s / day
Inclination23.482°
250.74°
224.30°
Physical characteristics
Dimensions6.388±0.074 km[5]
7.189±0.029 km[6]
7.99 km(calculated)[3]
710h[7]
0.23(assumed)[3]
0.350±0.147[5]
0.3776±0.0629[6]
S[3][8]
12.4[6] · 12.7[3] · 12.8[1] · 12.84±0.41[8]

3322 Lidiya, provisional designation1975 XY1, is a stony Phocaeaasteroid and potentiallyslow rotator from the inner regions of theasteroid belt, approximately 7 kilometers in diameter. It was discovered on 1 December 1975, by Soviet astronomerTamara Smirnova at theCrimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula.[9] The asteroid was named after Russian aviatorLidiya Zvereva.[2]

Orbit and classification

[edit]

Lidiya is a member of thePhocaea family (701),[4] a largeasteroid family ofinner-belt asteroids with a stony composition.[10]: 23  It orbits the Sun at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,351 days). Its orbit has aneccentricity of 0.22 and aninclination of 23° with respect to theecliptic.[1]

The body'sobservation arc begins with its first identification as1975 VJ6 at Nauchnij in November 1975, one month prior to its official discovery observation.[9]

Physical characteristics

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Lidiya has been characterized as a stonyS-type asteroid byPanSTARRS photometric survey.[8]

Potentially slow rotator

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In December 2012, a fragmentary rotationallightcurve of Lidiya was obtained from photometric observations at the Altimira Observatory (G76) in California. Lightcurve analysis gave arotation period of 710 hours with a brightness amplitude of 0.60magnitude (U=1).[7] This would make Lidiya one of theslowest rotators known to exist. However, since the lightcurve has such a poor quality rating, it is only apotentially slow rotator.

Diameter and albedo

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According to the survey carried out by theNEOWISE mission of NASA'sWide-field Infrared Survey Explorer, Lidiya measures 6.388 and 7.189 kilometers in diameter and its surface has analbedo of 0.350 and 0.3776, respectively.[5][6]

TheCollaborative Asteroid Lightcurve Link assumes an albedo of 0.23 – derived from25 Phocaea, the Phocaea family's largest member and namesake – and calculates a diameter of 7.99 kilometers based on anabsolute magnitude of 12.7.[3]

Naming

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Thisminor planet was named after Russian aviator Lidiya Vissarionovna Zvereva (1890–1916), the first Russian female pilot, who began flying in 1911. She was also an instructor of other pilots and involved in the construction of airplanes.[2] The official naming citation was published by theMinor Planet Center on 4 October 1990 (M.P.C. 17027).[11] The crater on Venus,Zvereva was also named in her honor in 1985.[a]

Notes

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  1. ^CraterZvereva,Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.

References

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  1. ^abcd"JPL Small-Body Database Browser: 3322 Lidiya (1975 XY1)" (2017-05-02 last obs.).Jet Propulsion Laboratory. Retrieved9 September 2017.
  2. ^abcSchmadel, Lutz D. (2007). "(3322) Lidiya".Dictionary of Minor Planet Names.Springer Berlin Heidelberg. p. 277.doi:10.1007/978-3-540-29925-7_3323.ISBN 978-3-540-00238-3.
  3. ^abcdef"LCDB Data for (3322) Lidiya". Asteroid Lightcurve Database (LCDB). Retrieved9 September 2017.
  4. ^ab"Asteroid 3322 Lidiya – Nesvorny HCM Asteroid Families V3.0".Small Bodies Data Ferret. Retrieved26 October 2019.
  5. ^abcMasiero, 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. Retrieved9 September 2017.
  6. ^abcdMainzer, 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. ^abBuchheim, Robert K. (October 2014)."Asteroid Lightcurves from Altimira Observatory".The Minor Planet Bulletin.41 (4):241–243.Bibcode:2014MPBu...41..241B.ISSN 1052-8091. Retrieved9 September 2017.
  8. ^abcVeres, 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. Retrieved9 September 2017.
  9. ^ab"3322 Lidiya (1975 XY1)".Minor Planet Center. Retrieved9 September 2017.
  10. ^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.
  11. ^"MPC/MPO/MPS Archive".Minor Planet Center. Retrieved9 September 2017.

External links

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Minor planets
Asteroid
Distant minor planet
Comets
Other
Authority control databasesEdit this at Wikidata
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