The Shaulladany family (010[1]) is a small collisional asteroid family of at least 13 known asteroids,[2] named for one of its members, the 16-kilometre (9.9 mi)-across asteroid 247341 Shaulladany (although its largest member is 37519 Amphios). It lies within the larger dynamical group of Jupiter trojans, a group of asteroids in an orbital resonance with Jupiter such that they stay about 60 degrees ahead of/behind the planet in its orbit at all times in the Lagrange points L4 and L5, with the Shaulladany family being part of the trailing cloud around L5, also known as the Trojan camp. All members of the family are dark (assumed to be C-type asteroids) with albedos of around 0.09.
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 Shaulladany family are both part of the wider Trojan dynamical group, and fragments of 37519 Amphios. The family is considered a non-catastrophic asteroid family because 37519 Amphios, its largest member, makes up a majority of the family's total mass, rather than simply being the largest of a number of fragments each making up a small fraction of the original destroyed asteroid.[3]
Large members
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- 37519 Amphios: 0.186 (49.5%)
- (76826) 2000 SW131: 0.0544 (14.5%)
- 247341 Shaulladany: 0.0241 (6.4%)
- (291807) 2006 KG89: 0.0178 (4.7%)
- (337804) 2001 UN216: 0.0142 (3.8%)
- (338343) 2002 WY19: 0.0104 (2.8%)
- (486695) 2013 WP63: 0.0098 (2.6%)
- (376867) 2001 TN222: 0.00927 (2.5%)
- (420313) 2011 YQ62: 0.00902 (2.4%)
- (347099) 2010 HO21: 0.00865 (2.3%)
- all other members: 0.0321 (8.5%)
| Name | Abs. Mag | Size (km) | proper a (AU) |
proper e |
proper i |
|---|---|---|---|---|---|
| 37519 Amphios | 11.15 | 33 | 5.2174 | 0.044 | 25.164 |
| (76826) 2000 SW131 | 12.04 | 21 | 5.2193 | 0.034 | 24.596 |
| 247341 Shaulladany | 12.63 | 16 | 5.2181 | 0.041 | 24.561 |
| (291807) 2006 KG89 | 12.85 | 18 | 5.2206 | 0.045 | 24.324 |
| (337804) 2001 UN216 | 13.01 | 15 | 5.2180 | 0.037 | 24.146 |
| (338343) 2002 WY19 | 13.24 | 10 | 5.2201 | 0.034 | 24.392 |
| (486695) 2013 WP63 | 13.28 | 9.8 | ? | 0.049 | 23.785 |
| (376867) 2001 TN222 | 13.32 | 13 | 5.2197 | 0.039 | 24.055 |
| (420313) 2011 YQ62 | 13.34 | 9.5 | ? | 0.031 | 24.067 |
| (347099) 2010 HO21 | 13.37 | 9.4 | 5.2178 | 0.042 | 24.878 |
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.