The Schubart family (002[1]) is a collisional asteroid family of at least 353 known asteroids,[2] named for its largest member, the 67-kilometre (42 mi)-across asteroid 1911 Schubart. It lies within the larger dynamical group of Hilda asteroids, a group of asteroids in the 3:2 orbital resonance with Jupiter. Like its namesake, all members of the family are dark P-type asteroids with albedos of around 0.06. Another asteroid family in the Hilda dynamical group is the Schubart family, named for its largest member, 1911 Schubart. All members of the family are dark P-type asteroids with albedos of around 0.04. Another asteroid family in the Hilda dynamical group is the Hilda family, named for its largest member, 153 Hilda.
An asteroid family is a group of physically-related asteroids usually created by a collision with an original larger asteroid, with the fragments continuing on similar orbits to the original. This is distinct from a dynamical group in that the members of a dynamical group only share similar orbits because of gravitational interactions with planets, which concentrate asteroids in a particular orbital range. Members of the Schubart family are both part of the wider Hilda dynamical group, and fragments of a single original asteroid. The family is considered a catastrophic asteroid family because even its largest member, 1911 Schubart, does not make up a majority of the family's mass.[3]
The family is fairly old, with an estimated age of 1.7±0.7 billion years.[4] Although this is old by the standards of typical asteroid families, the Hilda collisional family in the same orbital region is much older, possibly 4 billion years in age.[4]
Large members
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- 1911 Schubart: 3.2 (46.3%)
- 3923 Radzievskij: 0.293 (4.2%)
- 4230 van den Bergh: 0.256 (3.7%)
- (8376) 1992 OZ9: 0.245 (3.5%)
- (13035) 1989 UA6: 0.226 (3.3%)
- 9829 Murillo: 0.149 (2.2%)
- 8550 Hesiodos: 0.116 (1.7%)
- (15615) 2000 HU1: 0.104 (1.5%)
- (8913) 1995 YB2: 0.0698 (1.0%)
- (12307) 1991 UA: 0.0552 (0.8%)
- all other members: 2.19 (31.7%)
| Name | Abs. Mag | Size (km) | proper a (AU) |
proper e |
proper i |
|---|---|---|---|---|---|
| 1911 Schubart | 10.04 | 67 | 3.9659 | 0.191 | 2.916 |
| 3923 Radzievskij | 11.77 | 30 | 3.9661 | 0.196 | 2.874 |
| 4230 van den Bergh | 11.87 | 28 | 3.9661 | 0.197 | 2.853 |
| (8376) 1992 OZ9 | 11.90 | 28 | 3.9659 | 0.190 | 2.793 |
| (13035) 1989 UA6 | 11.96 | 27 | 3.9661 | 0.195 | 2.879 |
| 9829 Murillo | 12.26 | 26 | 3.9659 | 0.192 | 2.855 |
| 8550 Hesiodos | 12.44 | 25 | 3.9658 | 0.190 | 2.834 |
| (15615) 2000 HU1 | 12.52 | 22 | 3.9662 | 0.198 | 2.982 |
| (8913) 1995 YB2 | 12.81 | 20 | 3.9662 | 0.197 | 2.898 |
| (12307) 1991 UA | 12.98 | 20 | 3.9660 | 0.193 | 2.889 |
References
edit- ^ Nesvorny, D.; Broz, M.; Carruba, V. (2015). Identification and Dynamical Properties of Asteroid Families. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 978-0-8165-3213-1.
{{cite book}}:|journal=ignored (help) - ^ a b Nesvorný, David (14 August 2020). "Nesvorny HCM Asteroid Families | PDS SBN Asteroid/Dust Subnode". NASA Planetary Data System. doi:10.26033/6cg5-pt13. Retrieved 28 July 2024.
- ^ Holsapple, K.A.; Housen, K.R. (December 2019). "The catastrophic disruptions of asteroids: History, features, new constraints and interpretations". Planetary and Space Science. 179: 104724. Bibcode:2019P&SS..17904724H. doi:10.1016/j.pss.2019.104724. Retrieved 30 July 2024.
- ^ a b Vinogradova, T. A. (13 October 2015). "Identification of asteroid families in Trojans and Hildas". Monthly Notices of the Royal Astronomical Society. 454 (3): 2436–2440. doi:10.1093/mnras/stv2115. Retrieved 30 July 2024.