Asteroid families become visible as distinct concentrations when asteroids are plotted in the proper orbital element space (
i p vs a
p ). 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.
Contents 1 General properties 2 Origin and evolution 3 Identification of members, interlopers and background asteroids 3.1 Description 3.1.1 Hierarchical clustering method 4 Family types 4.1 Clusters, clumps, clans and tribes 5 List 5.1 Prominent families 5.2 All families 5.3 Other families or dynamical groups 6 See also 7 References 8 Further reading 9 External links General properties
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 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 "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
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 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 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 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 Prominent families
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 family, the Eos, Eunomia, Flora, Hungaria, Hygiea, Koronis, Nysa, Themis and Vesta family 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 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- Parent body · Notes Cat LoMP 001 Hilda family HIL 409 rim C 0.04 cat 002 Schubart family SHU 352 rim C 0.03 cat 003 Hungaria family H 2965 rim E 0.35 cat 004 Hektor family HEK 12 rim – – cat 005 Eurybates family ERY 218 rim 0.06 cat 006 unnamed family 006 7 rim – 0.06 — 007 [5] 007 1 inner ASP – 9007 James Bond — 008 Arkesilaos family ARK 37 rim – – cat 009 Ennomos family ENM 30 rim – 0.06 cat 010 unnamed family 010 13 rim – 0.09 (247341) 2001 UV209 (Jupiter trojan)— 401 Vesta family V 15252 inner V 0.35 cat 402 (Ariadne family) FLO 13786 inner S 0.30 Duponta family (1338), respectively.[6] [7] cat 403 Baptistina family BAP 2500 inner X 0.16 Belgica family (1052) at 100 m/s according to Carruba[7] cat 404 Massalia family MAS 6424 inner S 0.22 cat 405 (Hertha family; Eulalia family) NYS 19073 inner SFC 0.28 cat 406 Erigone family ERI 1776 inner CX 0.06 cat 407 Clarissa family CLA 179 inner X 0.05 302 Clarissa cat 408 Sulamitis family SUL 303 inner C 0.04 752 Sulamitis cat 409 Lucienne family LCI 142 inner S 0.22 1892 Lucienne cat 410 Euterpe family EUT 474 inner S 0.26 27 Euterpe cat 411 Datura family DAT 6 inner S 0.21 cat 412 Lucascavin family LCA 3 inner S – cat 413 Klio family KLI 330 inner C 0.07 84 Klio cat 414 Chimaera family CIM 108 inner CX 0.06 623 Chimaera cat 415 Chaldaea familySalli family ) CHL 132 inner C 0.07 cat 416 Svea family SVE 48 inner CX 0.06 329 Svea cat 417 unnamed family 417 9 inner – – (108138) 2001 GB11 — 701 Phocaea family PHO 1989 inner S 0.22 25 Phocaea cat 501 Juno family JUN 1684 middle S 0.25 cat 502 Eunomia family EUN 5670 middle S 0.19 15 Eunomia cat 504 Nemesis family(Liberatrix or Zdeněkhorský family) NEM 1302 middle C 0.05 (adj. Nemesian) ; also named after 58 Concordia (adj. Concordian) and 3827 Zdeněkhorský. Formerly Liberatrix family by Zappalà (1995) and Cellino (2002)cat 505 Adeona family ADE 2236 middle C 0.07 145 Adeona cat 506 (Roma family) MAR 2940 middle S 0.25 [8] cat 507 Padua family PAD 1087 middle X 0.10 [C] · 110 Lydia · adj. Paduan; Lydiancat 508 Aeolia family AEO 296 middle X 0.17 396 Aeolia cat 509 Chloris family CLO 424 middle C 0.06 cat 510 Misa family MIS 702 middle C 0.03 cat 511 Brangäne family BRG 195 middle S 0.10 606 Brangäne cat 512 Dora family DOR 1259 middle C 0.05 cat 513 Merxia family MRX 1215 middle S 0.23 cat 514 Agnia family AGN 2125 middle S 0.18 847 Agnia cat 515 Astrid family AST 489 middle C 0.08 cat 516 (Ceres family; Minerva family) GEF 2547 middle S 0.20 (adj. Cererian) after 1 Ceres; and Minerva (adj. Minervian) family after 93 Minerva (identified interloper)cat 517 König family KON 354 middle CX 0.04 3815 König cat 518 Rafita family RAF 1295 middle S 0.25 cat 519 Hoffmeister family HOF 1819 middle CF 0.04 1726 Hoffmeister cat 520 Iannini family IAN 150 middle S 0.32 4652 Iannini cat 521 Kazuya family KAZ 44 middle S 0.21 7353 Kazuya cat 522 Ino family INO 463 middle S 0.24 173 Ino cat 523 Emilkowalski family EMI 4 middle S 0.20 cat 524 Brugmansia family 524 3 middle S – cat 525 Schulhof family SHF 5 middle S 0.27 cat 526 unnamed family 526 58 middle C 0.06 (53546) 2000 BY6 — 527 Lorre family LOR 2 middle C 0.05 cat 528 Leonidas family LEO 135 middle CX 0.07 cat 529 Vibilia family VIB 180 middle C 0.06 cat 530 Phaeo family PAE 146 middle X 0.06 322 Phaeo cat 531 Mitidika family MIT 653 middle C 0.06 cat 532 Henan family HEN 1872 middle L 0.20 2085 Henan cat 533 Hanna family HNA 280 middle CX 0.05 1668 Hanna cat 534 Karma family KRM 124 middle CX 0.05 3811 Karma cat 535 Witt family WIT 1618 middle S 0.26 2732 Witt cat 536 Xizang family XIZ 275 middle – 0.12 2344 Xizang cat 537 Watsonia family WAT 99 middle L 0.13 729 Watsonia cat 538 Jones family (asteroids) JNS 22 middle T 0.05 3152 Jones cat 539 Aëria family AER 272 middle X 0.17 369 Aeria cat 540 Julia family (asteroids) JUL 33 middle S 0.19 89 Julia cat 541 Postrema family POS 108 middle CX 0.05 1484 Postrema cat 801 Pallas family PAL 128 middle B 0.16 cat 802 Gallia family GAL 182 middle S 0.17 148 Gallia cat 803 Hansa family HNS 1094 middle S 0.26 [9] cat 804 Gersuind family GER 415 middle S 0.15 686 Gersuind cat 805 Barcelona family BAR 306 middle S 0.25 945 Barcelona cat 806 Tina family TIN 96 middle X 0.34 1222 Tina cat 807 Brucato family BRU 342 middle CX 0.06 4203 Brucato cat 601 Hygiea family HYG 4854 outer CB 0.06 10 Hygiea cat 602 Themis family THM 4782 outer C 0.07 cat 603 Sylvia family SYL 255 outer X 0.05 cat 604 Meliboea family MEL 444 outer C 0.05 cat 605 (Lacrimosa family) KOR 5949 outer S 0.15 cat 606 Eos family EOS 9789 outer K 0.13 221 Eos cat 607 Emma family EMA 76 outer C 0.05 283 Emma cat 608 Brasilia family BRA 579 outer X 0.18 cat 609 Veritas family VER 1294 outer CPD 0.07 cat 610 Karin family KAR 541 outer S 0.21 [3] :8,18 cat 611 Naëma family NAE 301 outer C 0.08 cat 612 Tirela family TIR 1395 outer S 0.07 cat 613 Lixiaohua family LIX 756 outer CX 0.04 3556 Lixiaohua cat 614 Telramund family(Klytaemnestra family) TEL 468 outer S 0.22 cat 615 unnamed family 615 104 outer CX 0.17 (18405) 1993 FY12 — 616 Charis family CHA 808 outer C 0.08 627 Charis cat 617 Theobalda family THB 376 outer CX 0.06 cat 618 Terentia family TRE 79 outer C 0.07 1189 Terentia cat 619 Lau family LAU 56 outer S 0.27 10811 Lau cat 620 Beagle family BGL 148 outer C 0.09 [3] :7,8,18 cat 621 K-2 246 outer S 0.14 cat 622 Terpsichore family TRP 138 outer C 0.05 81 Terpsichore cat 623 Fringilla family FIR 134 outer X 0.05 709 Fringilla cat 624 Durisen family DUR 27 outer X 0.04 5567 Durisen cat 625 Yakovlev family YAK 67 outer C 0.05 5614 Yakovlev cat 626 San Marcello family SAN 144 outer X 0.19 7481 San Marcello cat 627 unnamed family 627 38 outer CX 0.05 (15454) 1998 YB3 — 628 unnamed family 628 248 outer S 0.10 (15477) 1999 CG1 — 629 unnamed family 629 58 outer S 0.21 (36256) 1999 XT17 — 630 Aegle family AEG 99 outer CX 0.07 96 Aegle cat 631 Ursula family URS 1466 outer CX 0.06 375 Ursula cat 632 Elfriede family ELF 63 outer C 0.05 618 Elfriede cat 633 Itha family ITH 54 outer S 0.23 918 Itha cat 634 Inarradas family INA 38 outer CX 0.07 3438 Inarradas cat 635 Anfimov family ANF 58 outer S 0.16 7468 Anfimov cat 636 Marconia family MRC 34 outer CX 0.05 1332 Marconia cat 637 unnamed family 637 64 outer CX 0.05 (106302) 2000 UJ87 — 638 Croatia family CRO 93 outer X 0.07 589 Croatia cat 639 Imhilde family IMH 43 outer CX 0.05 926 Imhilde cat 640 Gibbs family GBS 8 outer – – — – 641 Juliana family JLI 76 outer CX 0.05 816 Juliana cat 901 Euphrosyne family EUP 2035 outer C 0.06 31 Euphrosyne cat 902 Alauda family ALA 1294 outer B 0.07 702 Alauda cat 903 Ulla family ULA 26 outer X 0.05 cat 904 Luthera family(Kartvelia family) LUT 163 outer X 0.04 cat 905 Armenia family ARM 40 outer C 0.05 780 Armenia cat
Other families or dynamical groups 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 [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 :C D Candidate families (Nesvorný):[3] :19 929 Algunde, 1296 Andrée, 1646 Rosseland, 1942 Jablunka, 2007 McCuskey, 2409 Chapman, 4689 Donn, 6246 Komurotoru. (13698) 1998 KF35 , 539 Pamina, (300163) 2006 VW139 , 3567 Alvema, (7744) 1986 QA1 260 Huberta, 928 Hildrun, 2621 Goto, 1113 Katja, 8737 Takehiro, 46 Hestia 5 Astraea, 1044 Teutonia, 3110 Wagman, 4945 Ikenozenni, (7744) 1986 QA1 , 8905 Bankakuko, (25315) 1999 AZ8 , (28804) 2000 HC81 .
See also Proper orbital elements Category:Asteroid groups and families 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. ^ 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 . .mw-parser-output cite.citationfont-style:inherit.mw-parser-output .citation qquotes:"""""""'""'".mw-parser-output .citation .cs1-lock-free abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .citation .cs1-lock-subscription abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registrationcolor:#555.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration spanborder-bottom:1px dotted;cursor:help.mw-parser-output .cs1-ws-icon abackground:url("//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/Wikisource-logo.svg/12px-Wikisource-logo.svg.png")no-repeat;background-position:right .1em center.mw-parser-output code.cs1-codecolor:inherit;background:inherit;border:inherit;padding:inherit.mw-parser-output .cs1-hidden-errordisplay:none;font-size:100%.mw-parser-output .cs1-visible-errorfont-size:100%.mw-parser-output .cs1-maintdisplay:none;color:#33aa33;margin-left:0.3em.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-formatfont-size:95%.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-leftpadding-left:0.2em.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-rightpadding-right:0.2em^ "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0 . Retrieved 22 July 2017 . ^ This is a joke by Nesvorný et al. In their Table 2 the reference is to the 1995 film, "GoldenEye". ^ 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 . ^ 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 . ^ 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 . ^ The Hansa Family: A New High-Inclination Asteroid Family ^ 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 . ^ 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 . ^ 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 . ^ 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 Bendjoya, Philippe; and Zappalà, Vincenzo; "Asteroid Family Identification", in Asteroids III , pp. 613–618, University of Arizona Press (2002), V. Zappalà et al. "Physical and Dynamical Properties of Asteroid Families", in Asteroids III , pp. 619–631, University of Arizona Press (2002), A. Cellino et al. "Spectroscopic Properties of Asteroid Families", in Asteroids III , pp. 633–643, University of Arizona Press (2002), Hirayama, Kiyotsugu; "Groups of asteroids probably of common origin", Astronomical Journal , Vol. 31, No. 743, pp. 185-188 (October 1918). Nesvorný, David; Bottke Jr., William F.; Dones, Luke; and Levison, Harold F.; "The recent breakup of an asteroid in the main-belt region", Nature , Vol. 417, pp. 720-722 (June 2002). Zappalà, Vincenzo; Cellino, Alberto; Farinella, Paolo; and Knežević, Zoran; "Asteroid families I - Identification by hierarchical clustering and reliability assessment", Astronomical Journal , Vol. 100, p. 2030 (December 1990). Zappalà, Vincenzo; Cellino, Alberto; Farinella, Paolo; and Milani, Andrea; "Asteroid families II - Extension to unnumbered multiopposition asteroids", Astronomical Journal , Vol. 107, pp. 772-801 (February 1994) V. Zappalà et al. Asteroid Families: Search of a 12,487-Asteroid Sample Using Two Different Clustering Techniques , Icarus, Vol. 116, p. 291 (1995.) M. S. Kelley & M. J. Gaffey 9 Metis and 113 Amalthea: A Genetic Asteroid Pair , Icarus Vol. 144, p. 27 (2000). External links Asteroid Families Portal Asteroids
Main Notable asteroids Impact avoidance Tracking Capture Gravitational keyhole Earth-crosser Close approaches P–L Distribution Interior to Earthvulcanoids Mercury-crossers Venus-crossers TrojansVenus trojan Earth Mars Jupiter Uranus trojan Neptune trojan Aten Amor Apollo Apohele Earth-crossers Between Earth and the main beltMars crossers Mars trojans Outer Solar System, does not include distant minor planetsJupiter-crossers Jupiter trojan Classification
Orbital Spectral
Tholen S-type small classes A-type D-type J-type T-type Q-type R-type V-type SMASS A-type Q-type R-type K-type L-type S-type Sa Sq Sr Sk Sl small types T-type D-type Ld-type O-type V-type
Exploration Asteroid Redirect Mission Asteroids visited by spacecraft Human mission Colonization Lists Near-Earth Minor planets Lost Discovering observatories Space missions See also: Asteroids in fiction Comet Minor planet
Small Solar System bodies
Minor planets
Designation Groups List Moon Meanings of names Asteroid Aten asteroid Asteroid belt Family Jupiter trojan Near-Earth Spectral types Distant minor planet Centaur Damocloid Neptune trojan Detached Kuiper belt Oort cloud Scattered disc
Comets Extinct Great Halley-type Hyperbolic Long-period Lost Main-belt Near-parabolic Periodic Sungrazing Other
Clash Royale CLAN TAG#URR8PPP
