1089 Tama

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1089 Tama
1089Tama (Lightcurve Inversion).png
Lightcurve-based 3D-model of Tama
Discovery [1]
Discovered by O. Oikawa
Discovery site Tokyo Astronomical Obs.
Discovery date17 November 1927
Designations
(1089) Tama
PronunciationJapanese: [tama]
Named after
 Tama River [2]
(Japanese river)
1927 WB ·1930 ST
1952 HE4 ·A894 VA
A904 VD ·A919 HA
main-belt  ·(inner)
Flora [3]  · background [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 122.40 yr (44,708 days)
Aphelion 2.4951 AU
Perihelion 1.9327 AU
2.2139 AU
Eccentricity 0.1270
3.29 yr (1,203 days)
82.843°
0° 17m 57.12s / day
Inclination 3.7264°
71.489°
354.29°
Known satellites 1  [3] [5] [6]
Physical characteristics
Dimensions11.33±2.00 km [7]
12.2±1.6 km [8]
12.82 km (derived) [3]
12.92±0.6 km [9]
13.08±0.37 km [10]
13.082±0.373 km [10]
13.32±0.19 km [11]
4(dated) h [12]
16.4±0.1 h [13]
16.44 h [8]
16.444±0.001 h [14]
16.4442±0.0004 h [6] [13]
16.445±0.005 h [13]
16.45±0.05 h [13]
16.4530±0.0004 h [13]
16.464±0.004 h [15]
16.4655 h [16]
0.2048 (derived) [3]
0.216±0.029 [10]
0.2424±0.023 [9]
0.243±0.008 [11]
0.267±0.083 [8]
0.32±0.23 [7]
S (assumed) [3]
11.60 [9] [11]  ·11.63±0.0 [8]  ·11.70 [7] [10]  ·11.8 [1] [3]  ·11.86±0.85 [17]

    1089 Tama, provisional designation 1927 WB, is an elongated Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 12 kilometers in diameter.

    Contents

    It was discovered by Japanese astronomer Okuro Oikawa at the old Tokyo Astronomical Observatory ( 389 ) on 17 November 1927. [18] The asteroid was named after the Tama River in Japan. [2] Its minor-planet moon was discovered in December 2003 and measures approximately 9 kilometers. [6]

    Orbit and classification

    Tama is a member of the Flora family ( 402 ), a giant asteroid family and the largest family of stony asteroids in the main-belt. [3] It is, however, a non-family asteroid from the main belt's background population when applying the Hierarchical Clustering Method to its proper orbital elements. [4]

    The asteroid orbits the Sun in the inner main-belt at a distance of 1.9–2.5  AU once every 3 years and 3 months (1,203 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. [1] Tama was first identified as A894 VA at Heidelberg Observatory in November 1894. The body's observation arc begins with its identification as A904 VD at Heidelberg in November 1904, or 23 years prior to its official discovery observation at Tokyo. [18]

    Physical characteristics

    Tama is an assumed stony S-type asteroid. [3]

    Rotation period

    A large number of rotational lightcurves of Tama were obtained from photometric observations since it has been identified as a binary asteroid (see below). Lightcurve analysis gave a rotation period between 16.4 and 16.464 hours with a brightness variation between 0.08 and 0.41 magnitude ( U=2-/2-3-/3 ), superseding a period of 4 hours from a fragmentary lightcurve obtained in the 1990s ( U=1 ). [6] [8] [12] [13] [15]

    Tama appears to be somewhat elongated in shape. [6] LCDB's consolidated result gives a period of 16.44 hours and an amplitude of 0.41 magnitude ( U=3 ). [3]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, the Spitzer Space Telescope and the NEOWISE mission of the Wide-field Infrared Survey Explorer, Tama measures between 11.33 and 13.32 kilometers in diameter and its surface has an albedo between 0.216 and 0.32. [7] [8] [9] [10] [11]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2048 and a diameter of 12.82 kilometers based on an absolute magnitude of 11.8. [3]

    Satellite

    In 2004, it was announced that Tama has a minor-planet moon, provisionally designated S/2003 (1089) 1. The satellite was identified based on lightcurve observations with mutual occultation and eclipsing events from 24 December 2003 to 5 January 2004 by Raoul Behrend, René Roy, Claudine Rinner, Pierre Antonini, Petr Pravec, Alan Harris, Stefano Sposetti, Russell Durkee, and Alain Klotz. [6] [13] The moon measures approximately 9 kilometers in diameter. It may orbits 20 km away in a period of 16.4442 hours (synchronously). [3] [5] [6]

    Spin axis

    Tamas lightcurve has also been modeled. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue (UAPC) and the Palmer Divide Observatory, gave a concurring rotation period of 16.4655 hours. [16] Another modeled lightcurve using data from UAPC, the Palomar Transient Factory survey, and individual observers, gave a period of 16.4461 hours as well as two spin axes of (193.0°, 32.0°) and (9.0°, 28.0°) in ecliptic coordinates (λ, β). [19]

    Naming

    This minor planet was named after Tama River near the discovering Tokyo Astronomical Observatory ( 389 ) in Japan. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 103 ). [2]

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    References

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    12. 1 2 Sárneczky, K.; Szabó, Gy.; Kiss, L. L. (June 1999). "CCD observations of 11 faint asteroids". Astronomy and Astrophysics Supplement. 137 (2): 363–368. Bibcode:1999A&AS..137..363S. doi: 10.1051/aas:1999251 .
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    14. ↑ Behrend, R.; Bernasconi, L.; Roy, R.; Klotz, A.; Colas, F.; Antonini, P.; et al. (February 2006). "Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy". Astronomy and Astrophysics. 446 (3): 1177–1184. Bibcode:2006A&A...446.1177B. doi: 10.1051/0004-6361:20053709 .
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    17. ↑ 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 26 September 2017.
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    19. ↑ Hanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: 16. arXiv: 1301.6943 . Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701.
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