5592 Oshima

Last updated

5592 Oshima
Discovery  [1]
Discovered by K. Suzuki
T. Urata
Discovery site Toyota Obs.
Discovery date14 November 1990
Designations
(5592) Oshima
Named after
 Yoshiaki Oshima   [1]
(Japanese astronomer)
1990 VB4 ·1955 RA
main-belt   [1] [2]  ·(outer)
Veritas   [3] [4]
Orbital characteristics   [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 62.13 yr (22,693 d)
Aphelion 3.3830 AU
Perihelion 2.9610 AU
3.1720 AU
Eccentricity 0.0665
5.65 yr (2,063 d)
26.407°
0° 10m 28.2s / day
Inclination 8.4938°
231.63°
99.822°
Physical characteristics
Mean diameter
22.657±0.211  km [5] [6]
22.96±0.87 km [7]
24.6±0.2 km [8]
25.32 km (derived) [9]
25.43±2.5 km [10]
30.47±11.41 km [11]
38.39±4.47 km [3]
12.54±0.02  h [12]
0.0301±0.0059 [3]
0.04±0.09 [11]
0.0479(derived) [9]
0.06±0.01 [8]
0.0666±0.0040 [6]
0.0686±0.016 [10]
0.076±0.003 [5]
0.086±0.007 [7]
C (Pan-STARRS) [13]
C (SDSS-MOC) [14]
Caa (S3OS2-TH) [15]
Ch (S3OS2-BB) [15]
11.50 [7] [10]
11.68±0.37 [13]
11.7 [6] [8]
11.80 [11]
11.9 [2] [9]

    5592 Oshima, provisional designation 1990 VB4, is a Veritasian asteroid from the outer regions of the asteroid belt, approximately 25 kilometers (16 miles) in diameter. It was discovered on 14 November 1990, by astronomers Kenzo Suzuki and Takeshi Urata at the Toyota Observatory, and later named after Japanese astronomer Yoshiaki Oshima. [1] The carbonaceous C-type asteroid has a rotation period of 12.5 hours. [9]

    Contents

    Orbit and classification

    Oshima is a core member of the Veritas family ( 609 ), [3] [4] a young family of carbonaceous asteroids, that formed approximately 8.5±0.5 million years ago. The family is named after 490 Veritas and consists of nearly 1,300 members. [16] : 8, 23  Other members of this family include 1086 Nata and 2934 Aristophanes.

    This asteroid orbits the Sun in the outer main belt at a distance of 3.0–3.4  AU once every 5 years and 8 months (2,063 days; semi-major axis of 3.17 AU). Its orbit has an eccentricity of 0.07 and an inclination of 8° with respect to the ecliptic.[ citation needed ] The body's observation arc begins with its first observation as 1955 RA at Goethe Link Observatory in September 1955, more than 35 years prior to its official discovery observation at Toyota. [1]

    Physical characteristics

    Oshima has been characterized as a carbonaceous C-type asteroid by Pan-STARRS and in the SDSS-based taxonomy. [3] [9] [14] The Small Solar System Objects Spectroscopic Survey (S3OS2) it is classified as a Caa and hydrated Ch-type in the survey's Tholen- and SMASS-like taxonomy, respectively. [3] [15]

    Rotation period

    In September 2006, a rotational lightcurve of Oshima was obtained from photometric observations by French amateur astronomer Laurent Bernasconi. Lightcurve analysis gave a rotation period of 12.54±0.02 hours with a brightness amplitude of 0.28 magnitude ( U=2 ). [9] [12]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Oshima measures between 22.657 and 30.47 kilometers in diameter and its surface has an albedo between 0.04 and 0.086. [5] [6] [7] [8] [10] [11]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0479 and a diameter of 25.32 kilometers based on an absolute magnitude of 11.9. [9]

    Naming

    This minor planet was named by the second discoverer after Japanese astronomer Yoshiaki Oshima, a prolific discoverer of minor planets himself at the Gekko Observatory during the late 1990s. The official naming citation was published by the Minor Planet Center on 1 September 1993 ( M.P.C. 22511). [17]

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    References

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    2. 1 2 3 "JPL Small-Body Database Browser: 5592 Oshima (1990 VB4)" (2017-10-30 last obs.). Jet Propulsion Laboratory . Retrieved 14 June 2018.
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    14. 1 2 Carvano, J. M.; Hasselmann, P. H.; Lazzaro, D.; Mothé-Diniz, T. (February 2010). "SDSS-based taxonomic classification and orbital distribution of main belt asteroids". Astronomy and Astrophysics. 510: 12. Bibcode:2010A&A...510A..43C. doi: 10.1051/0004-6361/200913322 . Retrieved 30 October 2019. (PDS data set)
    15. 1 2 3 Lazzaro, D.; Angeli, C. A.; Carvano, J. M.; Mothé-Diniz, T.; Duffard, R.; Florczak, M. (November 2004). "S3OS2: the visible spectroscopic survey of 820 asteroids" (PDF). Icarus. 172 (1): 179–220. Bibcode:2004Icar..172..179L. doi:10.1016/j.icarus.2004.06.006 . Retrieved 9 June 2018.
    16. ↑ 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. S2CID   119280014.
    17. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 14 June 2018.
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