Английская Википедия:Asteroid family

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Шаблон:Short description

Файл:AsteroidIncAu.png
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

Файл:Asteroid proper elements i vs e.png
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 Шаблон:Dp.[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 asteroid 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).

Шаблон:Anchor Identification of members, interlopers and background asteroids

Шаблон:Redirect

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 (see above). 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

Файл:Asteroid osculating vs proper elements.png
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 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.

Шаблон:Anchor Hierarchical clustering method

Шаблон:Further

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.

Шаблон:Anchor List

Prominent families

Шаблон:Image frame

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 Шаблон:Section link.

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]Шаблон:Rp
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

Шаблон:Anchor

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]Шаблон:Rp 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]Шаблон:Rp

FIN Family Lbl # of Members Loc.
[note 1]
Taxonomy mean-
albedo
mean a mean e mean i Parent bodyШаблон:·Notes Cat LoMP
001 Hilda family HIL 409 rim C 0.04 3.965 0.174 8.92 153 Hilda; adj. Hildian; within the larger dynamical group with the same name.
(a–e–i: 3.7–4.2 AU; > 0.07; < 20°)
cat Шаблон:LoMP
002 Schubart family SHU 352 rim C 0.03 3.966 0.191 2.92 1911 Schubart (within the dynamical Hilda group) cat Шаблон:LoMP
003 Hungaria family H 2965 close E 0.35 1.944 0.078 20.87 434 Hungaria; located within the dynamical group of the same name.
(a–e–i: 1.78–2.0 AU; < 0.18; 16°–34°)
cat Шаблон:LoMP
004 Hektor family HEK 12 trojan 5.204 0.054 19.02 624 Hektor (Jupiter trojan) cat Шаблон:LoMP
005 Eurybates family ERY 218 trojan CP 0.06 5.204 0.044 7.42 3548 Eurybates (Jupiter trojan) cat Шаблон:LoMP
006 unnamed family 006 7 trojan 0.06 5.204 0.049 31.75 9799 Thronium (Jupiter trojan) Шаблон:LoMP
007 James Bond family[5] 007 1 A ASP 2.474 0.129 6.32 9007 James Bond Шаблон:LoMP
008 Arkesilaos family ARK 37 trojan 5.204 0.029 8.89 20961 Arkesilaos (Jupiter trojan) cat Шаблон:LoMP
009 Ennomos family ENM 30 trojan 0.06 5.204 0.041 26.79 4709 Ennomos (Jupiter trojan) cat Шаблон:LoMP
010 unnamed family 010 13 trojan 0.09 5.204 0.041 24.23 Шаблон:Mpl (Jupiter trojan) Шаблон:LoMP
401 Vesta family V 15252 A V 0.35 2.362 0.099 6.36 4 Vesta (adj. Vestian) cat Шаблон:LoMP
402 Flora family
Шаблон:Small
FLO 13786 A S 0.30 2.201 0.144 5.34 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 Шаблон:LoMP, respectively.[6][7] cat Шаблон:LoMP
403 Baptistina family BAP 2500 A X 0.16 2.264 0.149 6.00 298 Baptistina, merges with the Belgica family Шаблон:LoMP at 100 m/s according to Carruba[7] cat Шаблон:LoMP
404 Massalia family MAS 6424 A S 0.22 2.409 0.162 1.42 20 Massalia, adj. Massalian, a-e-i: (2.37 to 2.45; 0.12 to 0.21; 0.4 to 2.4) cat Шаблон:LoMP
405 Nysa–Polana complex
Шаблон:Small
NYS 19073 A SFC 0.28
0.06
2.423 0.174 3.04 44 Nysa/142 Polana also known as the Hertha family (135 Hertha). Includes the Eulalia family (495 Eulalia) cat Шаблон:LoMP
Шаблон:LoMP
406 Erigone family ERI 1776 A CX 0.06 2.367 0.210 4.74 163 Erigone, adj. Erigonian. Can be joined with the dynamically different Martes family into a single collisional family (Src). cat Шаблон:LoMP
407 Clarissa family CLA 179 A X 0.05 2.406 0.107 3.35 302 Clarissa cat Шаблон:LoMP
408 Sulamitis family SUL 303 A C 0.04 2.463 0.091 5.04 752 Sulamitis cat Шаблон:LoMP
409 Lucienne family LCI 142 A S 0.22 2.462 0.111 14.51 1892 Lucienne cat Шаблон:LoMP
410 Euterpe family EUT 474 A S 0.26 2.347 0.187 0.72 27 Euterpe cat Шаблон:LoMP
411 Datura family DAT 6 A S 0.21 2.235 0.156 5.21 1270 Datura; Recently formed family with members: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP cat Шаблон:LoMP
412 Lucascavin family LCA 3 A S 2.281 0.127 5.20 21509 Lucascavin; members: Шаблон:LoMP, Шаблон:LoMP cat Шаблон:LoMP
413 Klio family KLI 330 A C 0.07 2.362 0.193 9.38 84 Klio cat Шаблон:LoMP
414 Chimaera family CIM 108 A CX 0.06 2.460 0.155 14.65 623 Chimaera cat Шаблон:LoMP
415 Chaldaea family
(Шаблон:Small)
CHL 132 A C 0.07 2.376 0.236 11.60 313 Chaldaea; alt. named after 1715 Salli by Masiero cat Шаблон:LoMP
416 Svea family SVE 48 A CX 0.06 2.476 0.088 16.09 329 Svea cat Шаблон:LoMP
417 unnamed family 417 9 A 2.465 0.153 3.93 Шаблон:Mpl Шаблон:LoMP
701 Phocaea family PHO 1989 A S 0.22 2.400 0.228 23.41 25 Phocaea cat Шаблон:LoMP
501 Juno family JUN 1684 B S 0.25 2.669 0.232 13.34 3 Juno (adj. Junonian) cat Шаблон:LoMP
502 Eunomia family EUN 5670 B S 0.19 2.644 0.148 13.08 15 Eunomia cat Шаблон:LoMP
504 Nemesis family
Шаблон:Small
NEM 1302 C C 0.05 2.750 0.088 5.18 128 Nemesis (adj. Nemesian); also named after 58 Concordia (adj. Concordian) and 3827 Zdeněkhorský. Formerly Liberatrix family by Zappalà (1995) and Cellino (2002) cat Шаблон:LoMP
505 Adeona family ADE 2236 B C 0.07 2.673 0.169 11.71 145 Adeona cat Шаблон:LoMP
506 Maria family
Шаблон:Small
MAR 2940 B S 0.25 2.554 0.101 15.02 170 Maria; alternatively named after 472 Roma.[8] cat Шаблон:LoMP
507 Padua family
Шаблон:Small
PAD 1087 C X 0.10 2.747 0.035 5.09 363 Padua; also known as Lydia familyШаблон:Ref labelШаблон:·110 LydiaШаблон:·adj. Paduan; Lydian cat Шаблон:LoMP
508 Aeolia family AEO 296 C X 0.17 2.742 0.168 3.49 396 Aeolia cat Шаблон:LoMP
509 Chloris family CLO 424 C C 0.06 2.727 0.255 9.23 410 Chloris, adj. Chloridian cat Шаблон:LoMP
510 Misa family MIS 702 B C 0.03 2.658 0.178 2.26 569 Misa, adj. Misian cat Шаблон:LoMP
511 Brangäne family BRG 195 B S 0.10 2.587 0.179 9.64 606 Brangäne cat Шаблон:LoMP
512 Dora family DOR 1259 C C 0.05 2.797 0.198 7.83 668 Dora, adj. Dorian cat Шаблон:LoMP
513 Merxia family MRX 1215 C S 0.23 2.745 0.133 4.85 808 Merxia, adj. Merxian cat Шаблон:LoMP
514 Agnia family AGN 2125 C S 0.18 2.783 0.066 3.58 847 Agnia cat Шаблон:LoMP
515 Astrid family AST 489 C C 0.08 2.788 0.048 0.66 1128 Astrid, adj. Astridian cat Шаблон:LoMP
516 Gefion family
Шаблон:Small
GEF 2547 C S 0.20 2.784 0.129 9.01 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 Шаблон:LoMP
517 König family KON 354 B CX 0.04 2.571 0.139 8.85 3815 König cat Шаблон:LoMP
518 Rafita family RAF 1295 B S 0.25 2.547 0.173 7.74 1644 Rafita, adj. Rafitian (namesake is a suspected interloper; not listed in family); members Шаблон:LoMP and Шаблон:LoMP cat Шаблон:LoMP
519 Hoffmeister family HOF 1819 C CF 0.04 2.787 0.047 4.36 1726 Hoffmeister cat Шаблон:LoMP
520 Iannini family IAN 150 B S 0.32 2.644 0.267 12.19 4652 Iannini cat Шаблон:LoMP
521 Kazuya family KAZ 44 B S 0.21 2.568 0.141 14.56 7353 Kazuya cat Шаблон:LoMP
522 Ino family INO 463 C S 0.24 2.743 0.172 13.52 173 Ino cat Шаблон:LoMP
523 Emilkowalski family EMI 4 B S 0.20 2.599 0.178 17.42 14627 Emilkowalski; members: Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP cat Шаблон:LoMP
524 Brugmansia family 524 3 B S 2.620 0.179 2.80 16598 Brugmansia; members: Шаблон:LoMP and Шаблон:LoMP cat Шаблон:LoMP
525 Schulhof family SHF 5 B S 0.27 2.610 0.163 13.30 2384 Schulhof; members: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP cat Шаблон:LoMP
526 unnamed family 526 58 C C 0.06 2.721 0.173 14.35 Шаблон:Mpl Шаблон:LoMP
527 Lorre family LOR 2 C C 0.05 2.747 0.263 28.18 5438 Lorre; other member: Шаблон:LoMP cat Шаблон:LoMP
528 Leonidas family LEO 135 B CX 0.07 2.681 0.193 3.81 2782 Leonidas; identical to the Vibilia family: VIB (and listed as such); Шаблон:LoMP cat Шаблон:LoMP
529 Vibilia family VIB 180 B C 0.06 2.655 0.191 3.82 144 Vibilia; namesake only listed in family by Zappalà, but not by Nesvorý; identical to the Leonidas family: LEO. cat Шаблон:LoMP
530 Phaeo family PAE 146 C X 0.06 2.782 0.199 9.47 322 Phaeo cat Шаблон:LoMP
531 Mitidika family MIT 653 B C 0.06 2.587 0.247 12.50 2262 Mitidika (not listed in family itself); members: Шаблон:LoMP and Шаблон:LoMP cat Шаблон:LoMP
532 Henan family HEN 1872 B L 0.20 2.699 0.063 2.80 2085 Henan cat Шаблон:LoMP
533 Hanna family HNA 280 C CX 0.05 2.807 0.180 4.17 1668 Hanna cat Шаблон:LoMP
534 Karma family KRM 124 B CX 0.05 2.577 0.106 10.75 3811 Karma cat Шаблон:LoMP
535 Witt family WIT 1618 C S 0.26 2.760 0.030 5.79 2732 Witt cat Шаблон:LoMP
536 Xizang family XIZ 275 C 0.12 2.754 0.154 2.76 2344 Xizang cat Шаблон:LoMP
537 Watsonia family WAT 99 C L 0.13 2.760 0.122 17.33 729 Watsonia cat Шаблон:LoMP
538 Jones family (asteroids) JNS 22 B T 0.05 2.626 0.110 12.35 3152 Jones cat Шаблон:LoMP
539 Aëria family AER 272 B X 0.17 2.649 0.056 11.76 369 Aeria cat Шаблон:LoMP
540 Julia family (asteroids) JUL 33 B S 0.19 2.552 0.124 16.70 89 Julia cat Шаблон:LoMP
541 Postrema family POS 108 C CX 0.05 2.738 0.242 16.53 1484 Postrema cat Шаблон:LoMP
801 Pallas family PAL 128 C B 0.16 2.771 0.281 33.20 2 Pallas (adj. Palladian) cat Шаблон:LoMP
802 Gallia family GAL 182 C S 0.17 2.771 0.132 25.16 148 Gallia cat Шаблон:LoMP
803 Hansa family HNS 1094 B S 0.26 2.644 0.004 22.06 480 Hansa adj. Hansian; a-e-i: (~2.66; ~0.06; ~22.0°)[9] cat Шаблон:LoMP
804 Gersuind family GER 415 B S 0.15 2.589 0.175 17.34 686 Gersuind cat Шаблон:LoMP
805 Barcelona family BAR 306 B S 0.25 2.637 0.251 30.83 945 Barcelona cat Шаблон:LoMP
806 Tina family TIN 96 C X 0.34 2.793 0.082 20.76 1222 Tina cat Шаблон:LoMP
807 Brucato family BRU 342 B CX 0.06 2.605 0.132 28.90 4203 Brucato cat Шаблон:LoMP
601 Hygiea family HYG 4854 G CB 0.06 3.142 0.136 5.07 10 Hygiea cat Шаблон:LoMP
602 Themis family THM 4782 G C 0.07 3.134 0.152 1.08 24 Themis (adj. Themistian) cat Шаблон:LoMP
603 Sylvia family SYL 255 rim X 0.05 3.485 0.054 9.76 87 Sylvia; family within Cybele group cat Шаблон:LoMP
604 Meliboea family MEL 444 G C 0.05 3.119 0.186 14.54 137 Meliboea, adj. Meliboean cat Шаблон:LoMP
605 Koronis family
Шаблон:Small
KOR 5949 D S 0.15 2.869 0.045 2.15 158 Koronis, also named after 208 Lacrimosa cat Шаблон:LoMP
606 Eos family EOS 9789 E K 0.13 3.012 0.077 9.94 221 Eos cat Шаблон:LoMP
607 Emma family EMA 76 F C 0.05 3.046 0.113 9.09 283 Emma cat Шаблон:LoMP
608 Brasilia family BRA 579 D X 0.18 2.862 0.127 14.98 293 Brasilia, adj. Brazilian (namesake is a suspected interloper; not listed in family) cat Шаблон:LoMP
609 Veritas family VER 1294 G CPD 0.07 3.174 0.066 9.06 490 Veritas, adj. Veritasian; alt: Undina (Undinian) family after 92 Undina cat Шаблон:LoMP
610 Karin family KAR 541 D S 0.21 2.864 0.044 2.10 832 Karin. Recently formed family located within the Koronis family.[3]Шаблон:Rp cat Шаблон:LoMP
611 Naëma family NAE 301 D C 0.08 2.940 0.036 11.99 845 Naëma, adj. Naëmian cat Шаблон:LoMP
612 Tirela family
Шаблон:Small
TIR 1395 G S 0.07 3.116 0.195 17.06 1400 Tirela, alternatively named after 1040 Klumpkea (AstDyS) cat Шаблон:LoMP
613 Lixiaohua family
Шаблон:Small
LIX 756 G CX 0.04 3.153 0.201 10.06 3556 Lixiaohua; although member 3330 Gantrisch is both larger and lower numbered (src) cat Шаблон:LoMP
614 Telramund family
Шаблон:Small
TEL 468 E S 0.22 2.993 0.066 8.81 9506 Telramund; alternatively named after 179 Klytaemnestra by Masiero and by Milani cat Шаблон:LoMP
615 unnamed family 615 104 D CX 0.17 2.848 0.106 9.14 Шаблон:Mpl Шаблон:LoMP
616 Charis family CHA 808 D C 0.08 2.900 0.047 5.73 627 Charis cat Шаблон:LoMP
617 Theobalda family THB 376 G CX 0.06 3.178 0.263 14.05 778 Theobalda, adj. Theobaldian; a-e-i: (3.16 to 3.19; 0.24 to 0.27; 14 to 15) cat Шаблон:LoMP
618 Terentia family TRE 79 D C 0.07 2.932 0.072 11.11 1189 Terentia cat Шаблон:LoMP
619 Lau family LAU 56 D S 0.27 2.929 0.195 6.30 10811 Lau cat Шаблон:LoMP
620 Beagle family BGL 148 G C 0.09 3.155 0.154 1.34 656 Beagle. Recently formed family is located within the Themis family (all members are also listed as Themistians). Includes 7968 Elst–Pizarro.[3]Шаблон:Rp cat Шаблон:LoMP
621 Koronis family (II) K-2 246 D S 0.14 2.869 0.045 2.15 158 Koronis "second family" cat Шаблон:LoMP
622 Terpsichore family TRP 138 D C 0.05 2.854 0.182 8.23 81 Terpsichore cat Шаблон:LoMP
623 Fringilla family FIR 134 D X 0.05 2.914 0.093 16.68 709 Fringilla cat Шаблон:LoMP
624 Durisen family DUR 27 D X 0.04 2.943 0.185 16.19 5567 Durisen cat Шаблон:LoMP
625 Yakovlev family YAK 67 D C 0.05 2.870 0.290 7.89 5614 Yakovlev cat Шаблон:LoMP
626 San Marcello family SAN 144 D X 0.19 2.922 0.078 12.50 7481 San Marcello cat Шаблон:LoMP
627 unnamed family 627 38 D CX 0.05 2.868 0.219 16.02 Шаблон:Mpl Шаблон:LoMP
628 unnamed family 628 248 D S 0.10 2.850 0.081 5.12 Шаблон:Mpl Шаблон:LoMP
629 unnamed family 629 58 D S 0.21 2.939 0.118 10.73 Шаблон:Mpl Шаблон:LoMP
630 Aegle family AEG 99 F CX 0.07 3.052 0.190 16.48 96 Aegle cat Шаблон:LoMP
631 Ursula family URS 1466 G CX 0.06 3.128 0.098 16.21 375 Ursula cat Шаблон:LoMP
632 Elfriede family ELF 63 G C 0.05 3.189 0.061 15.87 618 Elfriede cat Шаблон:LoMP
633 Itha family ITH 54 D S 0.23 2.866 0.158 12.27 918 Itha cat Шаблон:LoMP
634 Inarradas family INA 38 F CX 0.07 3.050 0.184 14.51 3438 Inarradas cat Шаблон:LoMP
635 Anfimov family ANF 58 F S 0.16 3.044 0.089 3.48 7468 Anfimov cat Шаблон:LoMP
636 Marconia family MRC 34 F CX 0.05 3.063 0.097 2.58 1332 Marconia cat Шаблон:LoMP
637 unnamed family 637 64 G CX 0.05 3.109 0.180 3.46 Шаблон:Mpl Шаблон:LoMP
638 Croatia family CRO 93 G X 0.07 3.133 0.026 10.66 589 Croatia cat Шаблон:LoMP
639 Imhilde family IMH 43 E CX 0.05 2.983 0.237 14.59 926 Imhilde cat Шаблон:LoMP
640 Gibbs family GBS 8 E 3.004 0.023 10.34 331P/Gibbs "P/2012 F5 (Gibbs)". Other members include (20674), (140429), and (177075)
641 Juliana family JLI 76 E CX 0.05 3.004 0.144 13.12 816 Juliana cat Шаблон:LoMP
901 Euphrosyne family EUP 2035 G C 0.06 3.155 0.208 26.54 31 Euphrosyne cat Шаблон:LoMP
902 Alauda family ALA 1294 G B 0.07 3.194 0.021 21.66 702 Alauda cat Шаблон:LoMP
903 Ulla family ULA 26 rim X 0.05 3.543 0.050 17.96 909 Ulla; family within Cybele group cat Шаблон:LoMP
904 Luthera family
Шаблон:Small
LUT 163 G X 0.04 3.219 0.121 18.77 1303 Luthera; fam. is also named after 781 Kartvelia cat Шаблон:LoMP
905 Armenia family ARM 40 G C 0.05 3.117 0.070 18.19 780 Armenia cat Шаблон:LoMP

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: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP. 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]Шаблон:Rp
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.Шаблон:Ref label All members: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP.[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: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP.
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: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP.[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: Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP, Шаблон:LoMP and Шаблон:LoMP. 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).Шаблон:Ref label
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 Шаблон:LoMP to background.[3]Шаблон:Rp 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]Шаблон:Rp
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 (Шаблон:LoMP; Шаблон:LoMP), 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 Шаблон:LoMP.[3] Background asteroid: 301 Bavaria (both AstDyS-2 and Шаблон:LoMP). 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 (Шаблон:LoMP; Шаблон:LoMP).[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: Шаблон:Mpl; both are background asteroids according to AstDyS-2 and Шаблон:LoMP.
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 Шаблон:LoMP.[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]Шаблон:Rp
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

Notes

Шаблон:Reflist

References

Шаблон:Reflist

Further reading

Шаблон:Refbegin

Шаблон:Refend

External links

Шаблон:Asteroids Шаблон:Small Solar System bodies Шаблон:Portal bar

  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. 3,00 3,01 3,02 3,03 3,04 3,05 3,06 3,07 3,08 3,09 3,10 3,11 3,12 3,13 3,14 3,15 3,16 3,17 3,18 3,19 3,20 Ошибка цитирования Неверный тег <ref>; для сносок Nesvorny-2014 не указан текст
  4. Ошибка цитирования Неверный тег <ref>; для сносок Ferret не указан текст
  5. This is a joke by Nesvorný et al. In their Table 2 the reference is to the 1995 film, GoldenEye.
  6. 6,00 6,01 6,02 6,03 6,04 6,05 6,06 6,07 6,08 6,09 6,10 6,11 6,12 6,13 6,14 6,15 6,16 6,17 6,18 6,19 6,20 6,21 6,22 6,23 6,24 6,25 6,26 6,27 6,28 Ошибка цитирования Неверный тег <ref>; для сносок Milani-2014 не указан текст
  7. 7,0 7,1 Ошибка цитирования Неверный тег <ref>; для сносок Carruba-2013 не указан текст
  8. Ошибка цитирования Неверный тег <ref>; для сносок Masiero-2013 не указан текст
  9. The Hansa Family: A New High-Inclination Asteroid Family
  10. 10,00 10,01 10,02 10,03 10,04 10,05 10,06 10,07 10,08 10,09 10,10 10,11 10,12 10,13 10,14 10,15 10,16 10,17 10,18 10,19 10,20 10,21 10,22 10,23 10,24 10,25 10,26 10,27 Ошибка цитирования Неверный тег <ref>; для сносок Knezevic-2014 не указан текст
  11. 11,0 11,1 11,2 11,3 11,4 11,5 11,6 Ошибка цитирования Неверный тег <ref>; для сносок Zappala-family не указан текст
  12. 12,0 12,1 12,2 12,3 12,4 12,5 12,6 12,7 12,8 Ошибка цитирования Неверный тег <ref>; для сносок Roig-2008 не указан текст
  13. Ошибка цитирования Неверный тег <ref>; для сносок Milani-1993 не указан текст


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