Asteroid family

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An asteroid family is a group of minor planets that share similar orbital elements, such as semimajor axis, eccentricity, and orbital inclination. The members of the families are thought to be fragments of past asteroid collisions.

Plot of proper inclination vs. semi-major axis for numbered asteroids. Asteroid families are visible as distinct clumps. Prominent Kirkwood gaps divide the core region. (A, B+C, D, E+F+G)

Plot of proper inclination vs. eccentricity for numbered asteroids.

1 General properties
2 Origin and evolution
3 Identification of members and interlopers
4 Family types
5 List of families
6 See also
7 References
8 External links

[edit] General properties

Large, prominent families contain several hundred recognized asteroids (and many more smaller objects which may be either not-yet-analyzed, or not-yet-discovered). Small, compact families can have only about ten identified members. About 33% to 35% of asteroids in the main belt are family members.

There are about 20 to 30 reliably recognized families, with several tens of less certain groupings. Most asteroid families are found in the main asteroid belt, although several family-like groups such as the Pallas family, Hungaria family, and the Phocaea family lie at smaller semi-major axis or larger inclination than the main belt.

One family has been identified associated with the large Trans-Neptunian object 2003 EL₆₁ ^[1]. Some studies have tried to find evidence of collisional families among the trojan asteroids, but at present the evidence is inconclusive.

[edit] Origin and evolution

The families are thought to form as a result of collisions between asteroids. In many or most cases the parent body was shattered, but there are also several families which resulted from a large cratering event which did not disrupt the parent body (e.g. the Vesta, Pallas, Hygiea, and Massalia families). Such cratering families typically consist of a single large body and a swarm of asteroids that are much smaller. Some families (e.g. the Flora family) have complex internal structures which are not satisfactorily explained at the moment, but may be due to several collisions in the same region at different times.

Due to the method of origin, all the members have closely matching compositions for most families. Notable exceptions are those families (such as the Vesta family) which formed from a large differentiated parent body.

Asteroid families are thought to have lifetimes of the order of a billion years, depending on various factors (e.g. smaller asteroids are lost faster). This is significantly shorter than the Solar System's age, so few if any are relics of the early Solar System. Decay of families occurs both because of slow dissipation of the orbits due to perturbations from Jupiter or other large bodies, and because of collisions between asteroids which grind them down to small bodies. Such small asteroids then become subject to perturbations such as the Yarkovsky effect that can push them towards orbital resonances with Jupiter over time. Once there, they are relatively rapidly ejected from the asteroid belt. Tentative age estimates have been obtained for some families, ranging from hundreds of millions of years to less than several million years for e.g. the compact Karin family. Old families are thought to contain few small members, and this is the basis of the age determinations.

It is supposed that many very old families have lost all the smaller and medium-sized members, leaving only a few of the largest intact. A suggested example of such old family remains are the 9 Metis and 113 Amalthea pair. Further evidence for a large number of past families (now dispersed) comes from analysis of chemical ratios in iron meteorites. These show that there must have once been at least 50 to 100 parent bodies large enough to be differentiated, that have since been shattered to expose their cores and produce the actual meteorites (Kelley & Gaffey 2000).

[edit] Identification of members and interlopers

When the orbital elements of main belt asteroids are plotted (typically inclination vs. eccentricity, or vs. semi-major axis), a number of distinct concentrations are seen against the rather uniform background distribution of generic asteroids. These concentrations are the asteroid families.

Asteroid orbital elements: standard Keplerian on the left (families indistinguishable) vs. proper elements on the right (families visible).

Strictly speaking, families and their membership are identified by analysing the so-called proper orbital elements rather than the current osculating orbital elements, which regularly fluctuate on timescales of tens of thousands of years. The proper elements are related constants of motion that remain almost constant for times of at least tens of millions of years, and perhaps longer.

The Japanese astronomer Kiyotsugu Hirayama (1874-1943) pioneered the estimation of proper elements for asteroids, and first identified several of the most prominent families in 1918. In his honor, asteroid families are sometimes called Hirayama families. This particularly applies to the five prominent groupings discovered by him.

Present day computer-assisted searches have identified several tens of asteroid families. The most prominent algorithms have been the Hierarchical Clustering Method (HCM) which looks for groupings with small nearest-neighbour distances in orbital element space, and the Wavelet Analysis Method (WAM) which builds a density-of-asteroids map in orbital element space, and looks for density peaks.

The boundaries of the families are somewhat vague because at the edges they blend into the background density of asteroids in the main belt. For this reason the number of members even among discovered asteroids is usually only known approximately, and membership is uncertain for asteroids near the edges.

Additionally, some interlopers from the heterogeneous background asteroid population are expected even in the central regions of a family. Since the true family members caused by the collision are expected to have similar compositions, most such interlopers can in principle be recognised by spectral properties which do not match those of the bulk of family members. A prominent example is 1 Ceres, the largest asteroid, which is an interloper in the family once named after it (the Ceres family, now the Gefion family).

Spectral characteristics can also be used to determine the membership (or otherwise) of asteroids in the outer regions of a family, as has been used e.g. for the Vesta family, whose members have an unusual composition.

[edit] Family types

As previously mentioned, families caused by an impact that did not disrupt the parent body but only ejected fragments are called cratering families. Other terminology has been used to distinguish various types of groups which are less distinct or less statistically certain from the most prominent "nominal families" (or clusters). The term cluster is also used to describe a small asteroid family, such as the Karin Cluster^[2]. Clumps are groupings which have relatively few members but are clearly distinct from the background (e.g. the Juno clump). Clans are groupings which merge very gradually into the background density and/or have a complex internal structure making it difficult to decide whether they are one complex group or several unrelated overlapping groups (e.g. the Flora family has been called a clan). Tribes are groups that are less certain to be statistically significant against the background either because of small density or large uncertainty in the orbital parameters of the members.

[edit] List of families

Family Name	Named After	orbital elements			Size		Alternate Names
Family Name	Named After	a (AU)	e	i (°)	approx. % of asteroids	members in Zappalà HCM analysis^[A]	Alternate Names
The most prominent families within the main belt are:
Eos	221 Eos	2.99 to 3.03	0.01 to 0.13	8 to 12		480
Eunomia	15 Eunomia	2.53 to 2.72	0.08 to 0.22	11.1 to 15.8	5%	370
Flora	8 Flora	2.15 to 2.35	0.03 to 0.23	1.5 to 8.0	4-5%	590	Ariadne family after 43 Ariadne
Hygiea	10 Hygiea	3.06 to 3.24	0.09 to 0.19	3.5 to 6.8	1%	105
Koronis	158 Koronis	2.83 to 2.91	0 to 0.11	0 to 3.5		310
Maria	170 Maria	2.5 to 2.706		12 to 17		80
Nysa	44 Nysa	2.41 to 2.5	0.12 to 0.21	1.5 to 4.3		380	Hertha family after 135 Hertha
Themis	24 Themis	3.08 to 3.24	0.09 to 0.22	0 to 3		530
Vesta	4 Vesta	2.26 to 2.48	0.03 to 0.16	5.0 to 8.3	6%	240
Other notable main belt families^[C]:
Adeona	145 Adeona					65
Astrid	1128 Astrid					11
Bower	1639 Bower					13	Endymion family after 342 Endymion
Brasilia	293 Brasilia					14
Gefion	1272 Gefion	2.74 to 2.82	0.08 to 0.18	7.4 to 10.5	0.8%	89	Ceres family after 1 Ceres and Minerva family after 93 Minerva
Chloris	410 Chloris					24
Dora	668 Dora					78
Erigone	163 Erigone					47
Hilda	153 Hilda	3.7 to 4.2	>0.07	<20°	-
Karin	832 Karin					39^[B]
Lydia	110 Lydia					38
Massalia	20 Massalia	2.37 to 2.45	0.12 to 0.21	0.4 to 2.4	0.8%	47
Meliboea	137 Meliboea					15
Merxia	808 Merxia					28
Misa	569 Misa					26
Naëma	845 Naëma					7
Nemesis	128 Nemesis					29	Concordia family after 58 Concordia
Rafita	1644 Rafita					22
Veritas	490 Veritas					29	Undina family after 92 Undina
TNO families
2003 EL₆₁	(136108) 2003 EL₆₁	~43	~0.19	~28

Notes for table:

[A]: Mean of the "core" members found in HCM and WAM analyses by Zappala et al (1995), rounded to 2 significant digits. That analysis considered 12487 asteroids, but currently over 300,000 are known (an increase by a factor of over 25). Hence, the number of currently catalogued asteroids that are members of a given family is likely to be greater than the value in this column by a similar factor of roughly 25.
[B]: Reference elsewhere.
[C]: Most of these are families listed as "robustly" identified in Bendjoya and Zappala (2002). Exception: Karin family.

See also Category:Asteroid groups and families, which names some less prominent and uncertain groupings.

[edit] See also

[edit] References

^ Michael E. Brown, Kristina M. Barkume, Darin Ragozzine & Emily L. Schaller, A collisional family of icy objects in the Kuiper belt, Nature, 446, (March 2007), pp 294-296.
^ David Nesvorný, Brian L. Enke, William F. Bottke, Daniel D. Durda, Erik Ashaug & Derek C. Richardson Karin cluster formation by asteroid impact, Icarus 183, (2006) pp 296-311.