3322 Lidiya

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3322 Lidiya
Discovery  [1]
Discovered by T. Smirnova
Discovery site Crimean 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 arc 41.49 yr (15,153 days)
Aphelion 2.9105 AU
Perihelion 1.8738 AU
2.3921 AU
Eccentricity 0.2167
3.70 yr (1,351 days)
72.866°
0° 15m 59.04s / day
Inclination 23.482°
250.74°
224.30°
Physical characteristics
Dimensions6.388±0.074 km [5]
7.189±0.029 km [6]
7.99 km (calculated) [3]
710 h [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 designation 1975 XY1, is a stony Phocaea asteroid and potentially slow rotator from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered on 1 December 1975, by Soviet astronomer Tamara Smirnova at the Crimean Astrophysical Observatory in Nauchnij, on the Crimean peninsula. [9] The asteroid was named after Russian aviator Lidiya Zvereva. [2]

    Contents

    Orbit and classification

    Lidiya is a member of the Phocaea family ( 701 ), [4] a large asteroid family of inner-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 an eccentricity of 0.22 and an inclination of 23° with respect to the ecliptic. [1]

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

    Physical characteristics

    Lidiya has been characterized as a stony S-type asteroid by PanSTARRS photometric survey. [8]

    Potentially slow rotator

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

    Diameter and albedo

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

    The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.23 – derived from 25 Phocaea, the Phocaea family's largest member and namesake – and calculates a diameter of 7.99 kilometers based on an absolute magnitude of 12.7. [3]

    Naming

    This minor 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 the Minor Planet Center on 4 October 1990 ( M.P.C. 17027). [11] The crater on Venus, Zvereva was also named in her honor in 1985. [lower-alpha 1]

    Notes

    1. ↑ Crater Zvereva, Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 3322 Lidiya (1975 XY1)" (2017-05-02 last obs.). Jet Propulsion Laboratory . Retrieved 9 September 2017.
    2. 1 2 3 Schmadel, 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. 1 2 3 4 5 6 "LCDB Data for (3322) Lidiya". Asteroid Lightcurve Database (LCDB). Retrieved 9 September 2017.
    4. 1 2 "Asteroid 3322 Lidiya – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    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". The Astrophysical Journal. 791 (2): 11. arXiv: 1406.6645 . Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121 . Retrieved 9 September 2017.
    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 Buchheim, Robert K. (October 2014). "Asteroid Lightcurves from Altimira Observatory". The Minor Planet Bulletin. 41 (4): 241–243. Bibcode:2014MPBu...41..241B. ISSN   1052-8091 . Retrieved 9 September 2017.
    8. 1 2 3 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 9 September 2017.
    9. 1 2 "3322 Lidiya (1975 XY1)". Minor Planet Center. Retrieved 9 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. Retrieved 9 September 2017.
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