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Eurybates family

From Wikipedia, the free encyclopedia

TheEurybates family (005[1]) is a collisionalasteroid family of at least 218 known asteroids,[2] named for its largest member, the 64-kilometre (40 mi)-across asteroid3548 Eurybates. It lies within the larger dynamical group ofJupiter trojans, a group of asteroids in anorbital resonance withJupiter such that they stay about 60 degrees ahead of/behind the planet in its orbit at all times in theLagrange 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 darkC-type asteroids withalbedos 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 adynamical 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 widerTrojan 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 satelliteQueta 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 of1.05±0.36 billion years based on the modeled rate of family members escaping the trojan region over time.[5]

Large members

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Mass distribution of the Eurybates family (assuming similar densities)
The 10 brightest Eurybates family members[2]
NameAbs. MagSize (km)proper
a
(AU)
proper
e
proper
i
3548 Eurybates9.83645.29730.0447.422
5258 Rhoeo10.37535.28920.0597.027
8060 Anius11.05385.29220.0567.314
9818 Eurymachos11.12285.28600.0467.439
18060 Zarex11.17365.29250.0457.422
24380 Dorippe11.30325.29530.0447.348
24420 Thasos11.59225.30470.0497.240
13862 Elais11.74255.29280.0447.336
43436 Ansschut12.23215.29700.0527.165
28958 Binns12.25225.29650.0387.425

References

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  1. ^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)
  2. ^abNesvorný, David (14 August 2020)."Nesvorny HCM Asteroid Families | PDS SBN Asteroid/Dust Subnode".NASA Planetary Data System.doi:10.26033/6cg5-pt13. Retrieved28 July 2024.
  3. ^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. Retrieved30 July 2024.
  4. ^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.
  5. ^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. Retrieved1 August 2024.
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