825 Tanina

825 Tanina (prov. designation: A916 FH or 1916 ZL) is a stony background asteroid from the region of the Flora family, located in the inner part of the asteroid belt. It was discovered on 27 March 1916, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on Crimea.[1] The elongated S-type asteroid (SR) has a rotation period of 6.9 hours and measures approximately 13 kilometers (8.1 miles) in diameter. Any reference of the asteroid's name to a person is unknown.[2]

825 Tanina
Modelled shape of Tanina from its lightcurve
Discovery [1]
Discovered byG. Neujmin
Discovery siteSimeiz Obs.
Discovery date27 March 1916
Designations
(825) Tanina
Named after
unknown [2]
A916 FH · A904 UB
1916 ZL · 1904 UB
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc114.92 yr (41,974 d)
Aphelion2.3937 AU
Perihelion2.0578 AU
2.2257 AU
Eccentricity0.0755
3.32 yr (1,213 d)
112.91°
0° 17m 48.48s / day
Inclination3.3998°
101.41°
111.50°
Physical characteristics
Mean diameter
  • 11.02±0.7 km[7]
  • 13.06±0.38 km[8]
  • 13.423±0.150 km[9]
6.940±0.001 h[10]
  • (46.0°, 48.0°) (λ1/β1)[5]
  • (231.0°, 60.0°) (λ2/β2)[5]
  • 0.181±0.042[9]
  • 0.2624±0.038[7]
  • 0.278±0.018[8]
11.4[1][3]

    Orbit and classification

    Tanina is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method (HCM) by Nesvorný to its proper orbital elements.[5] In the 1995 HCM-analysis by Zappalà,[6] however, Tanina is a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[11]:23 In the HCM-analysis by Milani and Knežević (AstDys), it is also a background asteroid as this analysis does not recognize the Flora asteroid clan.[4] The asteroid orbits the Sun in the inner main-belt at a distance of 2.1–2.4 AU once every 3 years and 4 months (1,213 days; semi-major axis of 2.23 AU). Its orbit has an eccentricity of 0.08 and an inclination of 3° with respect to the ecliptic.[3]

    Discovery

    Tanina was discovered by Russian astronomer Grigory Neujmin at the Simeiz Observatory on Crimean peninsula on 27 March 1916. One week later, on 3 April 1916, it was independently discovered by Max Wolf at the Heidelberg Observatory in Germany. The Minor Planet Center only recognizes the first discoverer. The asteroid was first observed as A904 UB at Heidelberg on 17 October 1904, while the body's observation arc begins with Wolf's independent discovery observation.[1]

    Naming

    This minor planet was named "Tanina". Any reference of its name to a person or occurrence is unknown.[2]

    Unknown meaning

    Among the many thousands of named minor planets, Tanina is one of 120 asteroids, for which no official naming citation has been published. All of these asteroids have low numbers, the first one being 164 Eva. The last asteroid with a name of unknown meaning is 1514 Ricouxa. They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth.[12]

    Physical characteristics

    In the Tholen classification, Tanina is closest to a stony S-type asteroid, and somewhat similar to an uncommon R-type asteroid,[3] while in the SMASS classification by Bus–Binzel, Tanina is a common S-type asteroid.[13]

    Rotation period
    Lightcurve-based 3D-model of Tanina

    In February 2002, a rotational lightcurve of Tanina was obtained from photometric observations by Italian astronomer Andrea Ferrero at the Bigmuskie Observatory (B88). Lightcurve analysis gave a well-defined rotation period of 6.940±0.001 hours with a high brightness variation of 0.54±0.03 magnitude, indicative of an elongated, non-spherical shape (U=3). The result supersedes previous period determinations of 6.746±0.001 hours with an amplitude of 0.48±0.02 magnitude (U=2) by Wiesław Z. Wiśniewski from February 1992,[14] and 6.9398±0.0005 hours with an amplitude of 0.47±0.05 magnitude (U=2) by Agnieszka Kryszczyńska in May 1999.[15] In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a sidereal period 6.93981±0.00005 hours, as well as two spin axes at (46.0°, 48.0°) and (231.0°, 60.0°) in ecliptic coordinates (λ, β).[16]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Tanina measures (11.02±0.7), (13.06±0.38) and (13.423±0.150) kilometers in diameter and its surface has an albedo of (0.2624±0.038), (0.278±0.018) and (0.181±0.042), respectively.[7][8][9] The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.1508 from Petr Pravec's revised WISE data, and takes a diameter of 14.67 kilometers based on an absolute magnitude of 11.84.[13] Alternative mean-diameter measurements published by the WISE team include (12.690±0.350 km) and (14.611±0.068 km) with corresponding albedos of (0.275±0.042) and (0.1537±0.0333).[5][13]

    References
    1. "825 Tanina (A916 FH)". Minor Planet Center. Retrieved 14 March 2020.
    2. Schmadel, Lutz D. (2007). "(825) Tanina". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 76. doi:10.1007/978-3-540-29925-7_826. ISBN 978-3-540-00238-3.
    3. "JPL Small-Body Database Browser: 825 Tanina (A916 FH)" (2019-09-18 last obs.). Jet Propulsion Laboratory. Retrieved 14 March 2020.
    4. "Asteroid 825 Tanina – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 14 March 2020.
    5. "Asteroid 825 Tanina". Small Bodies Data Ferret. Retrieved 14 March 2020.
    6. Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 15 March 2020.} (PDS main page)
    7. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 14 March 2020.
    8. 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. Retrieved 14 March 2020. (online, AcuA catalog p. 153)
    9. Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System. Bibcode:2016PDSS..247.....M. Retrieved 14 March 2020.
    10. Ferrero, Andrea (July 2012). "Lightcurve Photometry of Six Asteroids" (PDF). Minor Planet Bulletin. 39 (3): 138–139. Bibcode:2012MPBu...39..138F. ISSN 1052-8091.
    11. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016.
    12. Schmadel, Lutz D. (2007). "Appendix 11 – Minor Planet Names with Unknown Meaning". Dictionary of Minor Planet Names – Fifth Revised and Enlarged revision. Springer Berlin Heidelberg. pp. 927–929. ISBN 978-3-540-00238-3.
    13. "LCDB Data for (825) Tanina". Asteroid Lightcurve Database (LCDB). Retrieved 14 March 2020.
    14. Wisniewski, W. Z.; Michałowski, T. M.; Harris, A. W.; McMillan, R. S. (April 1997). "Photometric Observations of 125 Asteroids". Icarus. 126 (2): 395–449. Bibcode:1997Icar..126..395W. doi:10.1006/icar.1996.5665. ISSN 0019-1035.
    15. Kryszczyńska, A.; Colas, F.; Polińska, M.; Hirsch, R.; Ivanova, V.; Apostolovska, G.; et al. (October 2012). "Do Slivan states exist in the Flora family?. I. Photometric survey of the Flora region" (PDF). Astronomy and Astrophysics. 546: A72. Bibcode:2012A&A...546A..72K. doi:10.1051/0004-6361/201219199. ISSN 0004-6361.
    16. Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738.
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