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Ennomos family

From Wikipedia, the free encyclopedia

TheEnnomos family (009[1]) is a small collisionalasteroid family of at least 28 known asteroids,[2] named for its largest member, the 81-kilometre (50 mi)-across asteroid4709 Ennomos. 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 Ennomos family being part of the trailing cloud around L5, also known as the Trojan camp. All members of the family are dark (assumed to beC-type asteroids) withalbedos 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 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 Ennomos family are both part of the widerTrojan dynamical group, and fragments of 4709 Ennomos. The family is considered a non-catastrophic asteroid family because 4709 Ennomos, 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]

The trojan1867 Deiphobus is a large interloper in the family's orbital region. A 2024 study found Deiphobus to have its own overlapping family to the Ennomos family, albeit with a slightly higher inclination.[4] As a result, some of the members included as part of the Ennomos family may actually belong to the Deiphobus family and vice versa.

Large members

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Mass distribution of the Ennomos family (assuming similar densities)
The 10 brightest Ennomos family members[2]
NameAbs. MagSize (km)proper
a
(AU)
proper
e
proper
i
4709 Ennomos8.66815.29650.03226.825
17492 Hippasos10.08545.33160.02827.611
(76867) 2000 YM510.49435.26160.02728.136
(55419) 2001 TF1911.25315.30690.03827.498
(36624) 2000 QA15711.67325.28510.02727.377
48373 Gorgythion12.17205.33470.03827.786
(98362) 2000 SA36312.51145.33080.03427.114
(131451) 2001 QD17412.60215.32100.04127.276
(77894) 2001 SY26312.63205.29960.03427.868
(247967) 2003 YD14912.63215.28410.02928.044

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. ^Vokrouhlický, David; Nesvorný, David; Brož, Miroslav; Bottke, William F.; Deienno, Rogerio; Fuls, Carson D.; Shelly, Frank C. (1 March 2024)."Orbital and Absolute Magnitude Distribution of Jupiter Trojans".The Astronomical Journal.167 (3): 138.arXiv:2401.15537.Bibcode:2024AJ....167..138V.doi:10.3847/1538-3881/ad2200.
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