Asteroid family


An asteroid family is a population of asteroids that share similar proper orbital elements, such as semi-major axis, eccentricity, and orbital inclination. The members of the families are thought to be fragments of past asteroid collisions. An asteroid family is a more specific term than asteroid group, whose members, while sharing some broad orbital characteristics, may be otherwise unrelated to each other.
Image:Asteroid proper elements i vs e.png|thumb|300px|Plot of proper inclination vs. eccentricity for numbered asteroids
Large prominent families contain several hundred recognized asteroids. Small, compact families may 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 dwarf planet. Some studies have tried to find evidence of collisional families among the trojan asteroids, but at present the evidence is inconclusive.

History

The Japanese astronomer Kiyotsugu Hirayama pioneered the estimation of proper elements for asteroids, and first identified several of the most prominent families in 1918. Kiyotsugu Hirayama initially identified the Koronis, Eos, and Themis families, and later recognized also the Flora and Maria families. In his honor, asteroid families are sometimes called Hirayama families. This particularly applies to the five prominent groupings discovered by him.

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. Such cratering families typically consist of a single large body and a swarm of asteroids that are much smaller. Some families 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 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. 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 as for 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 asteroid pair. Further evidence for a large number of past families 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.

Identification

Strictly speaking, families and their membership are identified by analysing the 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 at least tens of millions of years, and perhaps longer.

Membership

When the orbital elements of main belt asteroids are plotted, a number of distinct concentrations are seen against the rather uniform distribution of non-family background asteroids. These concentrations are the asteroid families. Interlopers are asteroids classified as family members based on their so-called proper orbital elements but having spectroscopic properties distinct from the bulk of the family, suggesting that they, contrary to the true family members, did not originate from the same parent body that once fragmented upon a collisional impact.

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".
The term cluster is also used to describe a small asteroid family, such as the Karin cluster. Clumps are groupings which have relatively few members but are clearly distinct from the background. 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. 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.

Hierarchical clustering method

Present day computer-assisted searches have identified more than a hundred asteroid families. The most prominent algorithms have been the hierarchical clustering method, which looks for groupings with small nearest-neighbour distances in orbital element space, and wavelet analysis, 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.
Spectral characteristics can also be used to determine the membership 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.

List

Prominent families

Among the many asteroid families, the following families are the most prominent ones in the asteroid belt. For the complete list, see below.
  • The Eos family
  • The Eunomia family is a family of S-type asteroids. It is the most prominent family in the intermediate asteroid belt and the 6th-largest family with approximately 1.4% of all main belt asteroids.
  • The Flora family is the 3rd-largest family. Broad in extent, it has no clear boundary and gradually fades into the surrounding background population. Several distinct groupings within the family, possibly created by later, secondary collisions. It has also been described as an asteroid clan.
  • The Hungaria family
  • The Hygiea family
  • The [|Koronis family]
  • The Nysa family. Alternatively named Hertha family after 135 Hertha.
  • The Themis family
  • The Vesta family

    All families

In 2015, a study identified 122 notable families with a total of approximately 100,000 member asteroids, based on the entire catalog of numbered minor planets, which consisted of almost 400,000 numbered bodies at the time '. The data has been made available at the "" website. The first column of this table contains the family identification number or family identifier number, which is an attempt for a numerical labeling of identified families, independent of their currently used name, as a family's name may change with refined observations, leading to multiple names used in literature and to subsequent confusion.
FINFamilyLbl# of MembersLoc.
Taxonomymean-
albedo
mean amean emean iParent bodyNotesCatLoMP
001Hilda familyHIL18rimC0.043.9650.1748.92153 Hilda; adj. Hildian; within the larger dynamical group with the same name.
cat
002Schubart familySHU531rimC0.033.9660.1912.921911 Schubart cat
003Hungaria familyH1870closeE0.351.9440.07820.87434 Hungaria; located within the dynamical group of the same name.
cat
004Hektor familyHEK16trojan 5.2040.05419.02624 Hektor cat
005Eurybates familyERY197trojan CP0.065.2040.0447.423548 Eurybates cat
006Thronium family00615trojan 0.065.2040.04931.759799 Thronium
007James Bond family0071AASP2.4740.1296.329007 James Bond
008Arkesilaos familyARK37trojan 5.2040.0298.8920961 Arkesilaos cat
009Ennomos familyENM30trojan 0.065.2040.04126.794709 Ennomos cat
010Shaulladany family01013trojan 0.095.2040.04124.23247341 Shaulladany
401Vesta familyV10612AV0.352.3620.0996.364 Vesta cat
402Flora family
FLO13786AS0.302.2010.1445.348 Flora, also named after 43 Ariadne; typical asteroid clan. Not a legitimate asteroid family according to Carruba and Milani, instead, the Florian core region is labelled Belgica family and Duponta family, respectively.cat
403Baptistina familyBAP176AX0.162.2640.1496.00298 Baptistina, merges with the Belgica family at 100 m/s according to Carrubacat
404Massalia familyMAS7820AS0.222.4090.1621.4220 Massalia, adj. Massalian, a-e-i: cat
405Nysa–Polana complex
NYS15983ASFC0.28
0.06
2.4230.1743.0444 Nysa/142 Polana also known as the Hertha family. Includes the Eulalia family cat
406Erigone familyERI1776ACX0.062.3670.2104.74163 Erigone, adj. Erigonian. Can be joined with the dynamically different Martes family into a single collisional family.cat
407Clarissa familyCLA236AX0.052.4060.1073.35302 Clarissacat
408Sulamitis familySUL193AC0.042.4630.0915.04752 Sulamitiscat
409Lucienne familyLCI142AS0.222.4620.11114.511892 Luciennecat
410Euterpe familyEUT474AS0.262.3470.1870.7227 Euterpecat
411Datura familyDAT6AS0.212.2350.1565.211270 Datura; Recently formed family with members:,,, and cat
412Lucascavin familyLCA3AS2.2810.1275.2021509 Lucascavin; members:, cat
413Klio familyKLI330AC0.072.3620.1939.3884 Kliocat
414Chimaera familyCIM108ACX0.062.4600.15514.65623 Chimaeracat
415Chaldaea family
CHL132AC0.072.3760.23611.60313 Chaldaea; alt. named after 1715 Salli by Masierocat
416Svea familySVE48ACX0.062.4760.08816.09329 Sveacat
417unnamed family4179A2.4650.1533.93
701Phocaea familyPHO1248AS0.222.4000.22823.4125 Phocaeacat
501Juno familyJUN1693BS0.252.6690.23213.343 Juno cat
502Eunomia familyEUN9856BS0.192.6440.14813.0815 Eunomiacat
504Nemesis family
NEM1302CC0.052.7500.0885.18128 Nemesis '; also named after 58 Concordia ' and 3827 Zdeněkhorský. Formerly Liberatrix family by Zappalà and Cellino cat
505Adeona familyADE2070BC0.072.6730.16911.71145 Adeonacat
506Maria family
MAR2958BS0.252.5540.10115.02170 Maria; alternatively named after 472 Roma.cat
507Padua family
PAD1087CX0.102.7470.0355.09363 Padua; also known as Lydia family110 Lydiaadj. Paduan; Lydiancat
508Aeolia familyAEO529CX0.172.7420.1683.49396 Aeoliacat
509Chloris familyCLO120CC0.062.7270.2559.23410 Chloris, adj. Chloridiancat
510Misa familyMIS647BC0.032.6580.1782.26569 Misa, adj. Misiancat
511Brangäne familyBRG325BS0.102.5870.1799.64606 Brangänecat
512Dora familyDOR1742CC0.052.7970.1987.83668 Dora, adj. Doriancat
513Merxia familyMRX1263CS0.232.7450.1334.85808 Merxia, adj. Merxiancat
514Agnia familyAGN3336CS0.182.7830.0663.58847 Agniacat
515Astrid familyAST548CC0.082.7880.0480.661128 Astrid, adj. Astridiancat
516Gefion family
GEF2428CS0.202.7840.1299.011272 Gefion, adj. Gefionian; a-e-i: ; also known as Ceres family ' after 1 Ceres; and Minerva family after 93 Minerva cat
517König familyKON578BCX0.042.5710.1398.853815 Königcat
518Rafita familyRAF775BS0.252.5470.1737.741644 Rafita, adj. Rafitian ; members and cat
519Hoffmeister familyHOF2095CCF0.042.7870.0474.361726 Hoffmeistercat
520Iannini familyIAN150BS0.322.6440.26712.194652 Ianninicat
521Kazuya familyKAZ44BS0.212.5680.14114.567353 Kazuyacat
522Ino familyINO463CS0.242.7430.17213.52173 Inocat
523Emilkowalski familyEMI4BS0.202.5990.17817.4214627 Emilkowalski; members:, and cat
524Brugmansia family5243BS2.6200.1792.8016598 Brugmansia; members: and cat
525Schulhof familySHF5BS0.272.6100.16313.302384 Schulhof; members:,,, cat
526unnamed family52681CC0.062.7210.17314.35
527Lorre familyLOR2CC0.052.7470.26328.185438 Lorre; other member: cat
528Leonidas family[|LEO]111BCX0.072.6810.1933.812782 Leonidas; identical to the Vibilia family: ; cat
529Vibilia familyVIB180BC0.062.6550.1913.82144 Vibilia; namesake only listed in family by Zappalà, but not by Nesvorý; identical to the Leonidas family: LEO.cat
530Phaeo familyPAE146CX0.062.7820.1999.47322 Phaeocat
531Mitidika familyMIT653BC0.062.5870.24712.502262 Mitidika ; members: and cat
532Henan familyHEN1872BL0.202.6990.0632.802085 Henancat
533Hanna familyHNA280CCX0.052.8070.1804.171668 Hannacat
534Karma familyKRM59BCX0.052.5770.10610.753811 Karmacat
535Witt familyWIT1618CS0.262.7600.0305.792732 Witt, alternatively named after 10955 Harig cat
536Xizang familyXIZ275C0.122.7540.1542.762344 Xizangcat
537Watsonia familyWAT83CL0.132.7600.12217.33729 Watsoniacat
538Jones family JNS22BT0.052.6260.11012.353152 Jonescat
539Aëria familyAER272BX0.172.6490.05611.76369 Aeriacat
540Julia family JUL33BS0.192.5520.12416.7089 Juliacat
541Postrema familyPOS108CCX0.052.7380.24216.531484 Postremacat
801Pallas familyPAL45CB0.162.7710.28133.202 Pallas cat
802Gallia familyGAL137CS0.172.7710.13225.16148 Galliacat
803Hansa familyHNS1162BS0.262.6440.00422.06480 Hansa adj. Hansian; a-e-i: cat
804Gersuind familyGER415BS0.152.5890.17517.34686 Gersuindcat
805Barcelona familyBAR346BS0.252.6370.25130.83945 Barcelonacat
806Tina familyTIN107CX0.342.7930.08220.761222 Tinacat
807Brucato familyBRU41BCX0.062.6050.13228.904203 Brucatocat
601Hygiea familyHYG3145GCB0.063.1420.1365.0710 Hygieacat
602Themis familyTHM5612GC0.073.1340.1521.0824 Themis cat
603Sylvia familySYL191rimX0.053.4850.0549.7687 Sylvia; family within Cybele groupcat
604Meliboea familyMEL444GC0.053.1190.18614.54137 Meliboea, adj. Meliboeancat
605Koronis family
KOR7390DS0.152.8690.0452.15158 Koronis, also named after 208 Lacrimosacat
606Eos familyEOS16038EK0.133.0120.0779.94221 Eoscat
607Emma familyEMA577FC0.053.0460.1139.09283 Emmacat
608Brasilia familyBRA845DX0.182.8620.12714.98293 Brasilia, adj. Brazilian cat
609Veritas familyVER2139GCPD0.073.1740.0669.06490 Veritas, adj. Veritasian; alt: Undina family after 92 Undinacat
610Karin familyKAR541DS0.212.8640.0442.10832 Karin. Recently formed family located within the Koronis family.cat
611Naëma familyNAE375DC0.082.9400.03611.99845 Naëma, adj. Naëmiancat
612Tirela family
TIR1815GS0.073.1160.19517.061400 Tirela, alternatively named after 1040 Klumpkea cat
613Lixiaohua family
LIX1241GCX0.043.1530.20110.063556 Lixiaohua; although member 3330 Gantrisch is both larger and lower numbered ]cat
614Telramund family
TEL513ES0.222.9930.0668.819506 Telramund; alternatively named after 179 Klytaemnestra by Masiero and by Milanicat
615unnamed family615159DCX0.172.8480.1069.14
616Charis familyCHA808DC0.082.9000.0475.73627 Chariscat
617Theobalda familyTHB574GCX0.063.1780.26314.05778 Theobalda, adj. Theobaldian; a-e-i: cat
618Terentia familyTRE80DC0.072.9320.07211.111189 Terentiacat
619Lau familyLAU56DS0.272.9290.1956.3010811 Laucat
620Beagle familyBGL148GC0.093.1550.1541.34656 Beagle. Recently formed family is located within the Themis family. Includes 7968 Elst–Pizarro.cat
621Koronis family K-2246DS0.142.8690.0452.15158 Koronis "second family"cat
622Terpsichore familyTRP138DC0.052.8540.1828.2381 Terpsichorecat
623Fringilla familyFIR134DX0.052.9140.09316.68709 Fringillacat
624Durisen familyDUR27DX0.042.9430.18516.195567 Durisencat
625Yakovlev familyYAK67DC0.052.8700.2907.895614 Yakovlevcat
626San Marcello familySAN144DX0.192.9220.07812.507481 San Marcellocat
627unnamed family62738DCX0.052.8680.21916.02
628unnamed family628248DS0.102.8500.0815.12
629unnamed family62958DA0.212.9390.11810.73
630Aegle familyAEG120FCX0.073.0520.19016.4896 Aeglecat
631Ursula familyURS731GCX0.063.1280.09816.21375 Ursulacat
632Elfriede familyELF97GC0.053.1890.06115.87618 Elfriedecat
633Itha familyITH54DS0.232.8660.15812.27918 Ithacat
634Inarradas familyINA43FCX0.073.0500.18414.513438 Inarradascat
635Anfimov familyANF49FS0.163.0440.0893.487468 Anfimovcat
636Marconia familyMRC34FCX0.053.0630.0972.581332 Marconiacat
637unnamed family63764GCX0.053.1090.1803.46
638Croatia familyCRO93GX0.073.1330.02610.66589 Croatiacat
639Imhilde familyIMH43ECX0.052.9830.23714.59926 Imhildecat
640Gibbs familyGBS8E3.0040.02310.34331P/Gibbs "P/2012 F5 ". Other members include,, and
641Juliana familyJLI76ECX0.053.0040.14413.12816 Julianacat
901Euphrosyne familyEUP1385GC0.063.1550.20826.5431 Euphrosynecat
902Alauda familyALA1294GB0.073.1940.02121.66702 Alaudacat
903Ulla familyULA37rimX0.053.5430.05017.96909 Ulla; family within Cybele groupcat
904Luthera family
LUT232GX0.043.2190.12118.771303 Luthera; fam. is also named after 781 Kartveliacat
905Armenia familyARM67GC0.053.1170.07018.19780 Armeniacat