Asteroid family

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Asteroid families become visible as distinct concentrations when asteroids are plotted in the proper orbital element space (ip vs ap). Some prominent families are the Vesta, Eunomia, Koronis, Eos, and Themis family located in different (colorized) regions of the asteroid belt.

An asteroid family is a population of asteroids that share similar proper orbital elements, such as semimajor 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.

General properties[edit]

Plot of proper inclination vs. eccentricity for numbered asteroids.

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 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 Haumea;[1] some studies have tried to find evidence of collisional families among the trojan asteroids, but at present the evidence is inconclusive.

Origin and evolution[edit]

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 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 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).

Identification of members, interlopers and background asteroids[edit]

"Interloper (asteroid)" redirects here. For other meanings of Interloper, see Interloper.

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 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.

Description[edit]

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

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 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.

Hierarchical clustering method[edit]

Further information: Hierarchical clustering

Present day computer-assisted searches have identified more than a hundred 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 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 (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.

Family types[edit]

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).

Clusters, clumps, clans and tribes[edit]

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.

List[edit]

Prominent families[edit]

Nysa familyVesta familyFlora familyEos familyKoronis familyEunomia familyHygiea familyThemis familyHungaria familyAsteroid family#All familiesAsteroid beltCircle frame.svg
  •   Nysa: 19,073 (4.8%)
  •   Vesta: 15,252 (3.8%)
  •   Flora: 13,786 (3.5%)
  •   Eos: 9,789 (2.5%)
  •   Koronis: 5,949 (1.5%)
  •   Eunomia: 5,670 (1.4%)
  •   Hygiea: 4,854 (1.2%)
  •   Themis: 4,782 (1.2%)
  •   Hungaria: 2,965 (0.7%)
  •   All other families: 21,500 (5.4%)
  •   Background: 295,000 (74.0%)
Distribution of the most prominent families, other families and background asteroids (up to number 398,000)[3]:23

Among the many asteroid families, the Eos, Eunomia, Flora, Hungaria, Hygiea, Koronis, Nysa, Themis and Vesta families are the most prominent ones in the asteroid belt. For a complete list, see § All families.

Eos family
The Eos family (adj. Eoan; 9,789 members, named after 221 Eos)
Eunomia family
The Eunomia family (adj. Eunomian; 5,670 known members, named after 15 Eunomia) 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.[3]:23
Flora family
The Flora family (adj. Florian; 13,786 members, named after 8 Flora) 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.
Hungaria family
The Hungaria family (adj. Hungarian; 2,965 members, named after 434 Hungaria)
Hygiea family
The Hygiea family (adj. Hygiean; 4,854 members, named after 10 Hygiea)
Koronis family
The Koronis family (adj. Koronian; 5,949 members, named after 158 Koronis)
Nysa family
The Nysa family (adj.Nysian; 19,073 members, named after 44 Nysa). Alternatively named Hertha family after 135 Hertha.
Themis family
The Themis family (adj. Themistian; 4,782 members, named after 24 Themis)
Vesta family
The Vesta family (adj. Vestian; 15,252 members, named after 4 Vesta)

All families[edit]

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 (see catalog index for a current listing of numbered minor planets).[3]:23 The data has been made available at the "Small Bodies Data Ferret";[4] the first column of this table contains the family identification number or family identifier number (FIN), 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.[3]:17

FIN Family Lbl # of Members Loc. Taxonomy mean-
albedo		 Parent body · Notes Cat LoMP
001 Hilda family HIL 409 rim C 0.04 153 Hilda; adj. Hildian; within the larger dynamical group with the same name.
(a–e–i: 3.7–4.2 AU; > 0.07; < 20°)		 cat list
002 Schubart family SHU 352 rim C 0.03 1911 Schubart (within the dynamical Hilda group) cat list
003 Hungaria family H 2965 rim E 0.35 434 Hungaria; located within the dynamical group of the same name.
(a–e–i: 1.78–2.0 AU; < 0.18; 16°–34°)		 cat list
004 Hektor family HEK 12 rim – – 624 Hektor (Jupiter trojan) cat list
005 Eurybates family ERY 218 rim CP 0.06 3548 Eurybates (Jupiter trojan) cat list
006 unnamed family 006 7 rim – 0.06 (9799) 1996 RJ (Jupiter trojan) — list
007 James Bond family[5] 007 1 inner ASP – 9007 James Bond — list
008 Arkesilaos family ARK 37 rim – – 20961 Arkesilaos (Jupiter trojan) cat list
009 Ennomos family ENM 30 rim – 0.06 4709 Ennomos (Jupiter trojan) cat list
010 unnamed family 010 13 rim – 0.09 (247341) 2001 UV209 (Jupiter trojan) — list
401 Vesta family V 15252 inner V 0.35 4 Vesta (adj. Vestian) cat list
402 Flora family
(Ariadne family)		 FLO 13786 inner S 0.30 8 Flora (adj. Florian), 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 (1338), respectively.[6][7] cat list
403 Baptistina family BAP 2500 inner X 0.16 298 Baptistina, merges with the Belgica family (1052) at 100 m/s according to Carruba[7] cat list
404 Massalia family MAS 6424 inner S 0.22 20 Massalia, adj. Massalian, a-e-i: (2.37 to 2.45; 0.12 to 0.21; 0.4 to 2.4) cat list
405 Nysa–Polana complex
(Hertha family; Eulalia family)		 NYS 19073 inner SFC 0.28
0.06		 44 Nysa/142 Polana also known as the Hertha family (135 Hertha). Includes the Eulalia family (495 Eulalia) cat (44)
(142)
406 Erigone family ERI 1776 inner CX 0.06 163 Erigone, adj. Erigonian cat list
407 Clarissa family CLA 179 inner X 0.05 302 Clarissa cat list
408 Sulamitis family SUL 303 inner C 0.04 752 Sulamitis cat list
409 Lucienne family LCI 142 inner S 0.22 1892 Lucienne cat list
410 Euterpe family EUT 474 inner S 0.26 27 Euterpe cat list
411 Datura family DAT 6 inner S 0.21 1270 Datura; Recently formed family with members: (60151), (90265), (203370), (215619) and (338309) cat list
412 Lucascavin family LCA 3 inner S – 21509 Lucascavin; members: (180255), (209570) cat list
413 Klio family KLI 330 inner C 0.07 84 Klio cat list
414 Chimaera family CIM 108 inner CX 0.06 623 Chimaera cat list
415 Chaldaea family
(Salli family)		 CHL 132 inner C 0.07 313 Chaldaea; alt. named after 1715 Salli by Masiero cat list
416 Svea family SVE 48 inner CX 0.06 329 Svea cat list
417 unnamed family 417 9 inner – – (108138) 2001 GB11 — list
701 Phocaea family PHO 1989 inner S 0.22 25 Phocaea cat list
501 Juno family JUN 1684 middle S 0.25 3 Juno (adj. Junonian) cat list
502 Eunomia family EUN 5670 middle S 0.19 15 Eunomia cat list
504 Nemesis family
(Liberatrix or Zdeněkhorský family)		 NEM 1302 middle C 0.05 128 Nemesis (adj. Nemesian); also named after 58 Concordia (adj. Concordian) and 3827 Zdeněkhorský. Formerly Liberatrix family by Zappalà (1995) and Cellino (2002) cat list
505 Adeona family ADE 2236 middle C 0.07 145 Adeona cat list
506 Maria family
(Roma family)		 MAR 2940 middle S 0.25 170 Maria; alternatively named after 472 Roma.[8] cat list
507 Padua family PAD 1087 middle X 0.10 363 Padua; also known as Lydia family[C] · 110 Lydia · adj. Paduan; Lydian cat list
508 Aeolia family AEO 296 middle X 0.17 396 Aeolia cat list
509 Chloris family CLO 424 middle C 0.06 410 Chloris, adj. Chloridian cat list
510 Misa family MIS 702 middle C 0.03 569 Misa, adj. Misian cat list
511 Brangäne family BRG 195 middle S 0.10 606 Brangäne cat list
512 Dora family DOR 1259 middle C 0.05 668 Dora, adj. Dorian cat list
513 Merxia family MRX 1215 middle S 0.23 808 Merxia, adj. Merxian cat list
514 Agnia family AGN 2125 middle S 0.18 847 Agnia cat list
515 Astrid family AST 489 middle C 0.08 1128 Astrid, adj. Astridian cat list
516 Gefion family
(Ceres family; Minerva family)		 GEF 2547 middle S 0.20 1272 Gefion, adj. Gefionian; a-e-i: (2.74 to 2.82; 0.08 to 0.18; 7.4 to 10.5); also known as Ceres family (adj. Cererian) after 1 Ceres; and Minerva (adj. Minervian) family after 93 Minerva (identified interloper) cat list
517 König family KON 354 middle CX 0.04 3815 König cat list
518 Rafita family RAF 1295 middle S 0.25 1644 Rafita, adj. Rafitian (namesake is a suspected interloper; not listed in family); members (1587) and (1658) cat list
519 Hoffmeister family HOF 1819 middle CF 0.04 1726 Hoffmeister cat list
520 Iannini family IAN 150 middle S 0.32 4652 Iannini cat list
521 Kazuya family KAZ 44 middle S 0.21 7353 Kazuya cat list
522 Ino family INO 463 middle S 0.24 173 Ino cat list
523 Emilkowalski family EMI 4 middle S 0.20 14627 Emilkowalski; members: (126761), (224559) and (256124) cat list
524 Brugmansia family 524 3 middle S – 16598 Brugmansia; members: (190603) and (218697) cat list
525 Schulhof family SHF 5 middle S 0.27 2384 Schulhof; members: (81337), (140600), (271044), (286239) cat list
526 unnamed family 526 58 middle C 0.06 (53546) 2000 BY6 — list
527 Lorre family LOR 2 middle C 0.05 5438 Lorre; other member: (208099) cat list
528 Leonidas family LEO 135 middle CX 0.07 2782 Leonidas; identical to the Vibilia family: VIB (and listed as such); (4793) cat list
529 Vibilia family VIB 180 middle C 0.06 144 Vibilia; namesake only listed in family by Zappalà, but not by Nesvorý; identical to the Leonidas family: LEO. cat list
530 Phaeo family PAE 146 middle X 0.06 322 Phaeo cat list
531 Mitidika family MIT 653 middle C 0.06 2262 Mitidika (not listed in family itself); members: (404) and (99) cat list
532 Henan family HEN 1872 middle L 0.20 2085 Henan cat list
533 Hanna family HNA 280 middle CX 0.05 1668 Hanna cat list
534 Karma family KRM 124 middle CX 0.05 3811 Karma cat list
535 Witt family WIT 1618 middle S 0.26 2732 Witt cat list
536 Xizang family XIZ 275 middle – 0.12 2344 Xizang cat list
537 Watsonia family WAT 99 middle L 0.13 729 Watsonia cat list
538 Jones family (asteroids) JNS 22 middle T 0.05 3152 Jones cat list
539 Aëria family AER 272 middle X 0.17 369 Aeria cat list
540 Julia family (asteroids) JUL 33 middle S 0.19 89 Julia cat list
541 Postrema family POS 108 middle CX 0.05 1484 Postrema cat list
801 Pallas family PAL 128 middle B 0.16 2 Pallas (adj. Palladian) cat list
802 Gallia family GAL 182 middle S 0.17 148 Gallia cat list
803 Hansa family HNS 1094 middle S 0.26 480 Hansa adj. Hansian; a-e-i: (~2.66; ~0.06; ~22.0°)[9] cat list
804 Gersuind family GER 415 middle S 0.15 686 Gersuind cat list
805 Barcelona family BAR 306 middle S 0.25 945 Barcelona cat list
806 Tina family TIN 96 middle X 0.34 1222 Tina cat list
807 Brucato family BRU 342 middle CX 0.06 4203 Brucato cat list
601 Hygiea family HYG 4854 outer CB 0.06 10 Hygiea cat list
602 Themis family THM 4782 outer C 0.07 24 Themis (adj. Themistian) cat list
603 Sylvia family SYL 255 outer X 0.05 87 Sylvia; family within Cybele group cat list
604 Meliboea family MEL 444 outer C 0.05 137 Meliboea, adj. Meliboean cat list
605 Koronis family
(Lacrimosa family)		 KOR 5949 outer S 0.15 158 Koronis, also named after 208 Lacrimosa cat list
606 Eos family EOS 9789 outer K 0.13 221 Eos cat list
607 Emma family EMA 76 outer C 0.05 283 Emma cat list
608 Brasilia family BRA 579 outer X 0.18 293 Brasilia, adj. Brazilian (namesake is a suspected interloper; not listed in family) cat list
609 Veritas family VER 1294 outer CPD 0.07 490 Veritas, adj. Veritasian; alt: Undina (Undinian) family after 92 Undina cat list
610 Karin family KAR 541 outer S 0.21 832 Karin. Recently formed family located within the Koronis family.[3]:8,18 cat list
611 Naëma family NAE 301 outer C 0.08 845 Naëma, adj. Naëmian cat list
612 Tirela family TIR 1395 outer S 0.07 1400 Tirela (Klumpkea) cat list
613 Lixiaohua family LIX 756 outer CX 0.04 3556 Lixiaohua cat list
614 Telramund family
(Klytaemnestra family)		 TEL 468 outer S 0.22 9506 Telramund; alternatively named after 179 Klytaemnestra by Masiero and by Milani cat list
615 unnamed family 615 104 outer CX 0.17 (18405) 1993 FY12 — list
616 Charis family CHA 808 outer C 0.08 627 Charis cat list
617 Theobalda family THB 376 outer CX 0.06 778 Theobalda, adj. Theobaldian; a-e-i: (3.16 to 3.19; 0.24 to 0.27; 14 to 15) cat list
618 Terentia family TRE 79 outer C 0.07 1189 Terentia cat list
619 Lau family LAU 56 outer S 0.27 10811 Lau cat list
620 Beagle family BGL 148 outer C 0.09 656 Beagle. Recently formed family is located within the Themis family (all members are also listed as Themistians). Includes 7968 Elst–Pizarro.[3]:7,8,18 cat list
621 Koronis family (II) K-2 246 outer S 0.14 158 Koronis "second family" cat list
622 Terpsichore family TRP 138 outer C 0.05 81 Terpsichore cat list
623 Fringilla family FIR 134 outer X 0.05 709 Fringilla cat list
624 Durisen family DUR 27 outer X 0.04 5567 Durisen cat list
625 Yakovlev family YAK 67 outer C 0.05 5614 Yakovlev cat list
626 San Marcello family SAN 144 outer X 0.19 7481 San Marcello cat list
627 unnamed family 627 38 outer CX 0.05 (15454) 1998 YB3 — list
628 unnamed family 628 248 outer S 0.10 (15477) 1999 CG1 — list
629 unnamed family 629 58 outer S 0.21 (36256) 1999 XT17 — list
630 Aegle family AEG 99 outer CX 0.07 96 Aegle cat list
631 Ursula family URS 1466 outer CX 0.06 375 Ursula cat list
632 Elfriede family ELF 63 outer C 0.05 618 Elfriede cat list
633 Itha family ITH 54 outer S 0.23 918 Itha cat list
634 Inarradas family INA 38 outer CX 0.07 3438 Inarradas cat list
635 Anfimov family ANF 58 outer S 0.16 7468 Anfimov cat list
636 Marconia family MRC 34 outer CX 0.05 1332 Marconia cat list
637 unnamed family 637 64 outer CX 0.05 (106302) 2000 UJ87 — list
638 Croatia family CRO 93 outer X 0.07 589 Croatia cat list
639 Imhilde family IMH 43 outer CX 0.05 926 Imhilde cat list
640 Gibbs family GBS 8 outer – – 331P/Gibbs "P/2012 F5 (Gibbs)" — –
641 Juliana family JLI 76 outer CX 0.05 816 Juliana cat list
901 Euphrosyne family EUP 2035 outer C 0.06 31 Euphrosyne cat list
902 Alauda family ALA 1294 outer B 0.07 702 Alauda cat list
903 Ulla family ULA 26 outer X 0.05 909 Ulla; family within Cybele group cat list
904 Luthera family
(Kartvelia family)		 LUT 163 outer X 0.04 1303 Luthera; fam. is also named after 781 Kartvelia cat list
905 Armenia family ARM 40 outer C 0.05 780 Armenia cat list

Other families or dynamical groups[edit]

Other asteroid families from miscellaneous sources (not listed in the above table), as well as non-asteroid families include:

Family Parent Cat Description
Aemilia family 159 Aemilia — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 62 members.
Alinda family 887 Alinda cat Alinda group described by projectpluto.com
Amneris family 871 Amneris cat Small family of 22 asteroids identified by Zappalà (1995).[11] Most members have been assigned to the encompassing complex of the Flora family by Nesvorný (2014).[3]
Anius family 8060 Anius — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 31 members.
Ashkova family 3460 Ashkova — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 59 members.
Astraea family 5 Astraea cat Large MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 6,169 members. Lowest-numbered members: (5), (91), (262), (355), (765) and (1121). Not a listed family by Zappalà (1995).[11] Considered a HCM-artifact by Nesvorný (2014) due to a resonant alignment (z1 = g + s − g6 − s6 = 0).[3]:19
Augusta family 254 Augusta cat Small family of 23 asteroids identified by Zappalà (1995).[11] Most members have been assigned to the Flora family by Nesvorný (2014).[3]
Ausonia family 63 Ausonia — Single member. Unsourced. Member of the Vesta family according to AstDyS-2 and Nesvorný (2014).[3]
Bontekoe family 10654 Bontekoe — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 13 members.
Brokoff family 6769 Brokoff — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 58 members.
Bower family 1639 Bower — Micro-family with 10 members as per Zappalà (1995). Adj. Bowerian. Alternative name Endymion (Endymionian) family after 342 Endymion.[C] All members: (1639), (3815), (8832), (14306), (15666), (22286), (32637), (85133), (120446) and (145685);[11] this family corresponds in large parts with the König family by Nesvorný (2014).[3]
Cindygraber family 7605 Cindygraber — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 19 members.
Clematis family 1101 Clematis cat MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 17 members. Subset of the large Alauda family as per Nesvorný (2014).[3] All members: (1101), (5360), (22044), (25982), (29963), (32240), (37628), (66174), (71688), (83362), (83790), (97516), (110030), (132961), (147858), (181960) and (223933).
Cybele group 65 Cybele cat Cybele group according to Asteroids, Meteorites, and Comets – by Linda T. Elkins-Tanton and projectpluto.com. Corresponding wiki-category lists a total of 32 members. Not a listed family in HCM by Zappalà (1995), Nesvorný (2014) and AstDyS-2 (Src), where these bodies are predominantly assigned to the background population.[11][3]
Dejanira family 157 Dejanira cat Micro-family with 5 members as per Zappalà (1995). All members: (157), (2290), (5276), (10779) and (17377).[11] All belong to the background population according to Nesvorný (2014).[3]
Devine family 3561 Devine — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 19 members.
Duponta family 1338 Duponta — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 133 members.
Epeios family 2148 Epeios — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Eumelos family 5436 Eumelos — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Euryalos family 4007 Euryalos — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Faïna family 751 Faïna cat Carbonaceous family with 12 identified members as per Zappalà (1995).[11] All members: (751), (2089), (2420), (3637), (3904), (5083), (8087), (10741), (10744), (11497), (12975) and (29086). Predominantly background population with 3 bodies belonging to the stony Maria family per Nesvorný (2014). Not a listed family at AstDyS-2 (Src)
Griqua group 1362 Griqua cat Griqua group (not a collisional family) described by projectpluto.com. A marginally unstable group of asteroids observed in the 2 :1 resonance with Jupiter.
Hanskya family 1118 Hanskya — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 116 members.
Haumea family Haumea (dwarf planet) cat This is a TNO-family. As of 2017, and current categorization, the family consists of 10 members (including parent body).[D]
Helio family 895 Helio — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 50 members.
Hestia family 46 Hestia cat Nesvorný moved family (formerly FIN 503) to candidate status, and (46) to background.[3]:19 Also background according to Milani and Knežević (AstDyS-2).
Higson family 3025 Higson — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 17 members.
Hippasos family 17492 Hippasos — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 7 members.
Huberta family 260 Huberta — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 26 members. Nesvorný moved family to candidate status.[3]:19
Kalchas family 4138 Kalchas — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Laodica family 507 Laodica cat Category with 2 members. 507 Laodica and 635 Vundtia are core members of the Eos family according to AstDyS-2 (507; 635) and background asteroid per Nesvorný (507; 635), respectively.[3]
Levin family 2076 Levin — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 1534 members.
Liberatrix family 125 Liberatrix cat 3 listed members. 125 Liberatrix is a background asteroid according to AstDyS-2, and a member of the Nemesis family according to Nesvorný.[3] Background asteroid: 301 Bavaria (both AstDyS-2 and Nesvorný). 9923 Ronaldthiel is a core member of the Agnia family at AstDyS-2.
Makhaon family 3063 Makhaon — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Marsili family 40134 Marsili — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 16 members.
Martes family 5026 Martes cat MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 481 members. Largest asteroids are members of the Erigone family according to Nesvorný (5026; 9879).[3]
Matterania family 883 Matterania — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 169 members.
Mecklenburg family 6124 Mecklenburg — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 78 members.
Melanthios family 12973 Melanthios — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Menelaus family 1647 Menelaus — Jupiter trojan family according Milani (1993).[13] Part of the Menelaus clan according to Roig and Gil-Hutton (2008).[12]
Nele family 1547 Nele — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 344 members.
Nocturna family 1298 Nocturna — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 186 members.
Nohavica family 6539 Nohavica cat Previously known as the "1982 QG" family. Second member: (9935) 1986 CP1; both are background asteroids according to AstDyS-2 and Nesvorný.
Podarkes family 13062 Podarkes — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Prokne family 194 Prokne — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 379 members.
Reginita family 1117 Reginita cat Claimed subgroup of the Flora family. Background asteroid according to both AstDyS-2 and Nesvorný.[3]
Sinden family 10369 Sinden — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 24 members.
Takehiro family 8737 Takehiro — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 57 members. Nesvorný moved family to candidate status.[3]:19
Telamon family 1749 Telamon — Jupiter trojan family according to Roig and Gil-Hutton (2008). Part of the Menelaus clan.[12]
Traversa family 5651 Traversa — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 56 members.
Univermoscow family 6355 Univermoscow — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 13 members.
Zhvanetskij family 5931 Zhvanetskij — MBA-family (AstDys) according to Milani and Knežević (2014).[6][10] Total of 23 members.
Legend:

See also[edit]

References[edit]

  1. ^ 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.
  2. ^ 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.
  3. ^ a b c d e f g h i j k l m n o p q r s t u v Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 23 June 2017.
  4. ^ "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 22 July 2017.
  5. ^ This is a joke by Nesvorný et al. In their Table 2 the reference is to the 1995 film, "GoldenEye".
  6. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab ac Milani, Andrea; Cellino, Alberto; Knezevic, Zoran; Novakovic, Bojan; Spoto, Federica; Paolicchi, Paolo (September 2014). "Asteroid families classification: Exploiting very large datasets" (PDF). Icarus. 239: 46–73. arXiv:1312.7702. Bibcode:2014Icar..239...46M. doi:10.1016/j.icarus.2014.05.039. Retrieved 17 April 2018.
  7. ^ a b Carruba, V.; Domingos, R. C.; Nesvorný, D.; Roig, F.; Huaman, M. E.; Souami, D. (August 2013). "A multidomain approach to asteroid families' identification" (PDF). Monthly Notices of the Royal Astronomical Society. 433 (3): 2075–2096. arXiv:1305.4847. Bibcode:2013MNRAS.433.2075C. doi:10.1093/mnras/stt884. Retrieved 5 December 2018.
  8. ^ Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Grav, T.; Nugent, C. R.; Stevenson, R. (June 2013). "Asteroid Family Identification Using the Hierarchical Clustering Method and WISE/NEOWISE Physical Properties" (PDF). The Astrophysical Journal. 770 (1): 22. arXiv:1305.1607. Bibcode:2013ApJ...770....7M. doi:10.1088/0004-637X/770/1/7. Retrieved 25 April 2018.
  9. ^ The Hansa Family: A New High-Inclination Asteroid Family
  10. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa ab Knezevic, Zoran; Milani, Andrea; Cellino, Alberto; Novakovic, Bojan; Spoto, Federica; Paolicchi, Paolo (July 2014). "Automated Classification of Asteroids into Families at Work". Complex Planetary Systems. 310: 130–133. Bibcode:2014IAUS..310..130K. doi:10.1017/S1743921314008035. Retrieved 17 April 2018.
  11. ^ a b c d e f g V. Zappala (1995). "Asteroid Dynamical Families – EAR-A-5-DDR-FAMILY-V4.1". NASA Planetary Data System. Retrieved 7 November 2018.
  12. ^ a b c d e f g h i Roig, F.; Ribeiro, A. O.; Gil-Hutton, R. (June 2008). "Taxonomy of asteroid families among the Jupiter Trojans: comparison between spectroscopic data and the Sloan Digital Sky Survey colors" (PDF). Astronomy and Astrophysics. 483 (3): 911–931. arXiv:0712.0046. Bibcode:2008A&A...483..911R. doi:10.1051/0004-6361:20079177. Retrieved 29 June 2018.
  13. ^ Milani, Andrea (October 1993). "The Trojan asteroid belt: Proper elements, stability, chaos and families". Celestial Mechanics and Dynamical Astronomy. 57: 59–94. Bibcode:1993CeMDA..57...59M. doi:10.1007/BF00692462. ISSN 0923-2958. Retrieved 29 June 2018.

Further reading[edit]

External links[edit]

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