Eurybates family
The Eurybates family (005[1]) is a collisional asteroid family of at least 218 known asteroids,[2] named for its largest member, the 64-kilometre (40 mi)-across asteroid 3548 Eurybates. 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 Eurybates family being part of the leading cloud around L4, also known as the Greek camp. All members of the family are dark C-type asteroids with albedos of around 0.05.
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 Eurybates family are both part of the wider Trojan dynamical group, and fragments of 3548 Eurybates. The family is considered a catastrophic asteroid family because 3548 Eurybates, its largest member, makes up only a quarter of the family's mass.[3]
The family's exact age is not known, though it has been constrained to under 3.7 billion years, because simulations show that 3548 Eurybates's satellite Queta would be very unlikely to survive to the modern day if it had formed earlier than this.[4] A more recent study suggested an age of 1.05±0.36 billion years based on the modeled rate of family members escaping the trojan region over time.[5]
Large members
[edit]
- 3548 Eurybates: 2.62 (26.5%)
- 5258 Rhoeo: 1.24 (12.6%)
- 8060 Anius: 0.486 (4.9%)
- 9818 Eurymachos: 0.441 (4.5%)
- 18060 Zarex: 0.412 (4.2%)
- 24380 Dorippe: 0.344 (3.5%)
- 24420 Thasos: 0.23 (2.3%)
- 13862 Elais: 0.187 (1.9%)
- 43436 Ansschut: 0.0952 (1.0%)
- 28958 Binns: 0.0926 (0.9%)
- all other members: 3.73 (37.8%)
| Name | Abs. Mag | Size (km) | proper a (AU) |
proper e |
proper i |
|---|---|---|---|---|---|
| 3548 Eurybates | 9.83 | 64 | 5.2973 | 0.044 | 7.422 |
| 5258 Rhoeo | 10.37 | 53 | 5.2892 | 0.059 | 7.027 |
| 8060 Anius | 11.05 | 38 | 5.2922 | 0.056 | 7.314 |
| 9818 Eurymachos | 11.12 | 28 | 5.2860 | 0.046 | 7.439 |
| 18060 Zarex | 11.17 | 36 | 5.2925 | 0.045 | 7.422 |
| 24380 Dorippe | 11.30 | 32 | 5.2953 | 0.044 | 7.348 |
| 24420 Thasos | 11.59 | 22 | 5.3047 | 0.049 | 7.240 |
| 13862 Elais | 11.74 | 25 | 5.2928 | 0.044 | 7.336 |
| 43436 Ansschut | 12.23 | 21 | 5.2970 | 0.052 | 7.165 |
| 28958 Binns | 12.25 | 22 | 5.2965 | 0.038 | 7.425 |
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. Retrieved 28 July 2024.
{{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.
- ^ Marschall, Raphael; Nesvorný, David; Deienno, Rogerio; Wong, Ian; Levison, Harold F.; Bottke, William F. (1 October 2022). "Implications for the Collisional Strength of Jupiter Trojans from the Eurybates Family". The Astronomical Journal. 164 (4): 167. arXiv:2208.10505. Bibcode:2022AJ....164..167M. doi:10.3847/1538-3881/ac8d6b.
- ^ Holt, Timothy R; Nesvorný, David; Horner, Jonathan; King, Rachel; Marschall, Raphael; Kamrowski, Melissa; Carter, Brad; Brookshaw, Leigh; Tylor, Christopher (11 July 2020). "Stability of Jovian Trojans and their collisional families". Monthly Notices of the Royal Astronomical Society. 495 (4): 4085–4097. arXiv:2005.03635. doi:10.1093/mnras/staa1348. Retrieved 1 August 2024.