Minor planet moon

243 Ida and its moon Dactyl as imaged by the Galileo spacecraft in 1993.

762 Pulcova and satellite as seen with adaptive optics in 2000.

A minor planet moon is an astronomical body that orbits a minor planet as its natural satellite. It is thought that many asteroids and Kuiper belt objects may possess moons, in some cases quite substantial in size. Discoveries of minor-planet moons (and binary objects, in general) are important because the determination of their orbits provides estimates on the mass and density of the primary, allowing insights of their physical properties that is generally not otherwise possible.^[1] As of October 2009^[update], there are 180 minor planets known to have moons.^[2]

Terminology

In addition to the terms satellite and moon, the term binary is sometimes used for minor planets with moons (or triple for minor planets with two moons). If one object is much bigger it is usually referred to as the primary and its companion as secondary. The term double asteroid is sometimes used for systems in which the asteroid and its moon are roughly the same size, while binary tends to be used independently from the relative sizes of the components. When binary minor planets are similar in size, the Minor Planet Center (MPC) refers to them as "binary companions" instead of referring to the smaller body as a satellite.^[3] A good example of a true binary is the 90 Antiope system, identified in August 2000.^[4] Small satellites are often referred to as moonlets.^[1][5]

Discovery milestones

As of October 2009^[update], 190 minor planet moons had been discovered,^[2] 67 in the asteroid belt (5 with two satellites),^[2] 4 Jupiter trojans, 37^[2] to 41^[6] near-Earth objects and 9 Mars-crossers.^[2] There are also 63 known moons of trans-Neptunian objects.^[2][6]

As early as 1978, following a stellar occultation, 532 Herculina had been suggested to have a moon^[7] and there were reports of other asteroids having companions (usually referred to as satellites) in the following years. A letter in Sky & Telescope magazine at this time pointed to pairs of large craters (e.g. the Clearwater Lakes in Quebec) also suggesting asteroids having companions.

However, it was not until 1993 that the first asteroid moon was confirmed when the Galileo probe discovered Dactyl orbiting 243 Ida. The second was discovered around 45 Eugenia in 1998.^[8] In 2001, 617 Patroclus and its same-sized companion Menoetius became the first known binary system in the trojan population.^[9] The first trans-Neptunian binary, 1998 WW₃₁ was optically resolved in 2002.^[10]

Triple systems

In 2005, the asteroid 87 Sylvia was discovered to have two moons, making it the first known triple asteroid.^[11] This was followed by the discovery of a second moon orbiting 45 Eugenia.^[12] Also in 2005, the Kuiper belt object (KBO) Haumea was discovered to have two moons, making it the second KBO after Pluto known to have more than one moon. Other known triple systems include: 3749 Balam (March 2008),^[13] 216 Kleopatra (September 2008),^[14] and 93 Minerva (August 2009).^[15]

Commonality

The data about the populations of binary objects are still patchy. In addition to the inevitable observational bias (dependence on the distance from Earth, size, albedo and separation of the components) the frequency appears to be different among different categories of objects. Among asteroids, an estimated 2% would have satellites. Among trans-Neptunian objects (TNO), an estimated 11% are believed to be binary or multiple objects, but three of the four known large TNO (75%) have at least one satellite.

More than 20 binaries are known in each of the main groupings: near-Earth asteroids, main-belt asteroids, and trans-Neptunians, not including numerous claims based solely on light-curve variation.

No binaries have been found so far among centaurs with semi-major axis smaller than Neptune.^[16] However, using an extended definition of Centaurs, as the objects on unstable orbits with the perihelion inside the orbit of Neptune, the first binary centaur, 42355 Typhon (previously known as 2002 CR₄₆), was identified in 2006.^[17]

Origin

The origin of minor-planet moons is not currently known with certainty, and a variety of theories exist. A widely accepted theory is that minor-planet moons are formed from debris knocked off of the primary by an impact. Other pairings may be formed when a small object is captured by the gravity of a larger one.

Formation by collision is constrained by the angular momentum of components i.e. by the masses and their separation. Close binaries fit this model (e.g. Pluto–Charon). Distant binaries however, with components of comparable size, are unlikely to have followed this scenario, unless considerable mass has been lost in the event.

The distances of the components for the known binaries vary from a few hundreds of kilometres (243 Ida, 3749 Balam) to more than 3000 km (379 Huenna) for the asteroids. Among TNOs, the known separations vary from 3,000 to 50,000 km.^[16]

Populations

What is "typical" for a binary system tends to depend on its location in the Solar System (presumably because of different modes of origin and lifetimes of such systems in different populations of minor planets).^[18]

• Among near-Earth asteroids, satellites tend to orbit at distances of the order of 3–7 primary radii, and have diameters two to several times smaller than the primary. Since these binaries are all inner-planet crossers, it is thought that tidal stresses that occurred when the parent object passed close to a planet may be responsible for the formation of many of them, although collisions are thought to also be a factor in the creation of these satellites.
• Among main-belt asteroids, the satellites are usually much smaller than the primary (a notable exception being 90 Antiope), and orbit around 10 primary radii away. Many of the binary systems here are members of asteroid families, and a good proportion of satellites are expected to be fragments of a parent body whose disruption after an asteroid collision produced both the primary and satellite.
• Among trans-Neptunian objects, it is common for the two orbiting components to be of comparable size, and for the semi-major axis of their orbits to be much larger − about 100 to 1000 primary radii. A significant proportion of these binaries are expected to be primordial.

Dwarf planets

Among the dwarf planets, it is 90 percent certain that Ceres has no moons larger than 1 km in size, assuming that they would have the same albedo as Ceres itself.^[19]

Pluto has four moons. Its largest moon Charon is more than half as large as Pluto itself, and large enough to orbit a point outside Pluto's surface. In effect, each orbits the other, forming a binary system informally referred to as a double-dwarf-planet. Pluto's three other moons, Nix, Hydra, and P4, are far smaller and orbit the Pluto–Charon system.

Makemake has no known moons. A satellite having 1% Makemake's brightness would have been detected if it had been located at an angular distance from Makemake farther than 0.4 arcseconds (0.0001 degrees).^[20]

Eris has one known moon, Dysnomia. Its radius, based on its brightness, is estimated to be 50 to 125 km.^[21]

Haumea has two moons with radii estimated around 155 km (Hiʻiaka) and 85 km (Namaka).

List of minor planets with moons

Near-Earth objects

Radar images of asteroid (66391) 1999 KW₄ and its moon. The 'streaks' on the image are the moon's trail as it moved while the images were created.

Near-Earth encounter of asteroid (136617) 1994 CC in June 2009 showing two moons.

Name	Type	Diameter (km) (or dimensions)	Name of moon	Diameter of moon (km) (or dimensions)	Separation (km)
1862 Apollo	Apollo	1.7	S/2005 (1862) 1	0.08	3
3671 Dionysus	Amor	1.5	S/1997 (3671) 1	0.4	2.2
5381 Sekhmet	Aten	1	S/2003 (5381) 1	0.3	1.54 ± 0.12
7088 Ishtar	Amor	1.5?	S/2006 (7088) 1	?	?
(31345) 1998 PG	Amor	0.9	S/2001 (31345) 1	0.3	1.5
(35107) 1991 VH	Apollo	1.2	S/2001 (35107) 1	0.5	3.2
65803 Didymos	Amor	0.8	S/2003 (65803) 1	0.15 ± 0.05	1.1
69230 Hermes	Apollo	0.4	S/2003 (69230) 1	0.4	1
(136617) 1994 CC	Apollo	0.7	? 2	both ~0.05	?
S/1999 (137170) 1	0.8	7.0
(162000) 1990 OS	Apollo	0.3	S/2003 (1990 OS) 1	0.045	0.6
1994 XD	Apollo	1?	S/2005 (1994 XD) 1	?	?
2004 DC	Apollo	0.3	S/2006 (2004 DC) 1	?	?
2005 AB	Amor	1.2?	S/2005 (2005 AB) 1	0.3	2.5?
edit] Mars crossers Name Diameter (km) (or dimensions) Name of moon Diameter of moon (km) (or dimensions) Separation (km) 1139 Atami 7 S/2005 (1139) 1 5 15? 2044 Wirt 7 S/2006 (2044) 1 2  ? (5407) 1992 AX 4 S/2001 (5407) 1 1.2 6.8 edit] Main-belt asteroids Name Diameter (km) (or dimensions) Name of moon Diameter of moon (km) (or dimensions) Separation (km) 22 Kalliope (215×180×150) Linus 38 ± 6 1,065 ± 8 41 Daphne 174.0 S/2008 (41) 1 <2 443 45 Eugenia (305×220×145) Petit-Prince (Eugenia I) 13 ± 1 1,184 ± 12 S/2004 (45) 1 ~6 ~700(?) 87 Sylvia (385×265×230) Remus (Sylvia II) 7 ± 2 706 ± 5 Romulus (Sylvia I) 18 ± 4 1,356 ± 5 90 Antiope 110±16 S/2000 (90) 1 110 ± 16 170 ± 1 93 Minerva 140 S/2009 (93) 1 4 630? S/2009 (93) 2 3 380? 107 Camilla (285×205×170) ± 20 S/2001 (107) 1 11 ± 2 1,235 ± 16 121 Hermione (254×125) S/2002 (121) 1 12 ± 4 768 ± 11 130 Elektra (215×155) S/2003 (130) 1 6 ± 2 1,252 ± 30 216 Kleopatra 217×94×81 Alexhelios (Kleopatra I) 5 650 Cleoselene (Kleopatra II) 3 380 243 Ida (59.8×25.4×18.6) Dactyl (Ida I) (1.6×1.4×1.2) 108 283 Emma 148.1 ± 4.6 S/2003 (283) 1 12 596 ± 3 379 Huenna 92.3 ± 1.7 S/2003 (379) 1 7 3,400 ± 11 702 Alauda 194.73 ± 3.2 S/2007 (702) 1 5.5 900 762 Pulcova 137.1 ± 3.2 S/2000 (762) 1 20 810 809 Lundia ~7–10 S/2005 (809) 1 ~7–10 ~10–20 854 Frostia 13.7 ± 5.6 S/2004 (854) 1 10 ~25 1089 Tama 12.9 S/2003 (1089) 1 9 20 1313 Berna 11 S/2004 (1313) 1 11 35 1338 Duponta 8–19 S/2007 (1338) 1 ~3?  ? 1509 Esclangona 12 S/2003 (1509) 1 4 140 1717 Arlon 9? S/2006 (1717) 1  ? 18? 2006 Polonskaya 10 S/2005 (2006) 1  ?  ? 2478 Tokai 10? S/2007 (2478) 1 7?  ? 2486 Metsähovi[22] 12? S/2007 (2486) 1  ?  ? 2754 Efimov 7? S/2006 (2754) 1  ? 12? 3073 Kursk 8? S/2007 (3073) 1  ?  ? 3309 Brorfelde 6? S/2005 (3309) 1  ?  ? 3703 Volkonskaya 3 S/2003 (3703) 1 1.2  ? 3749 Balam 7 S/2002 (3749) 1 1.5 310 ± 20 S/2008 (3749) 1 3 ~20 3782 Celle 6 S/2003 (3782) 1 2.5 30 3982 Kastel  ? S/2005 (3982) 1  ?  ? 4029 Bridges 10 S/2006 (4029) 1  ?  ? 4492 Debussy 10 S/2004 (4492) 1  ? 25 4674 Pauling 8 S/2004 (4674) 1 2.5 250 4786 Tatianina 8? S/2006 (4786) 1  ?  ? (5477) 1989 UH2 ~7 S/2005 (5477) 1 2.5 15 5905 Johnson 5 S/2005 (5905) 1 2  ? 6084 Bascom 9? S/2006 (6084) 1 3.5? 32? 6244 Okamoto 7? S/2006 (6244) 1 1.7? 15? 9069 Hovland 3 S/2004 (9069) 1 0.9  ? 9260 Edwardolson ~4 S/2005 (9260) 1  ?  ? 9617 Grahamchapman 5? S/2006 (9617) 1 1.4?  ? 11264 Claudiomaccone 4 S/2003 (11264) 1 1.2  ? edit] Jupiter trojans Name Diameter (km) (or dimensions) Name of moon Diameter of moon (km) (or dimensions) Separation (km) 617 Patroclus 121.8 ± 3.2 Menoetius (Patroclus I) 112.6 ± 3.2 685 ± 40 624 Hektor (363×207) S/2006 (624) 1 15 1,000? Trans-Neptunian objects Name Type Diameter (km) (or dimensions) Name of moon Diameter of moon (km) (or dimensions) Separation (km) 134340 Pluto Plutino 2306±20 Charon (Pluto I) 1207±3 19,571±4 Nix (Pluto II) 44–130 48,675±120 S/2011 P 1 (Pluto IV) 13–34 59,000±2,000 Hydra (Pluto III) 44–130 64,780±90 (26308) 1998 SM165 Plutino 221? S/2001 (26308) 1 88 11,310 ± 110 42355 Typhon SDO 134 Echidna (Typhon I) 78 1,300? (47171) 1999 TC36 Plutino A1=286 +45 −38 A2=265 +41 −35 S/2001 (47171) 1 139 +22 −18 7411 ± 12 (48639) 1995 TL8 SDO 352 S/2005 (48639) 1 161 420 50000 Quaoar Cubewano <1100 Weywot (Quaoar I) 96?  ? (55637) 2002 UX25 Cubewano 649 S/2007 (55637) 1 205  ? 58534 Logos Cubewano 80 Zoe (Logos I) 66 8,010 ± 80 2:5 resonance 151? S/2007 (60621) 1 115? 1,200 65489 Ceto SDO 172 Phorcys (Ceto I) 134 1,840 66652 Borasisi Cubewano 166 Pabu (Borasisi I) 137 4,660 ± 170 (79360) 1997 CS29 Cubewano 305 S/2005 (79360) 1 292 2300 88611 Teharonhiawako Cubewano 176 ± 20 Sawiskera (Teharonhiawako I) 122 ± 14 27,300 ± 343 90482 Orcus Plutino 946 Vanth (Orcus I) 262 ± 170 8,700 (119979) 2002 WC19 1:2 resonance 420? S/2007 (119979) 1  ?  ? 120347 Salacia Cubewano 580? Actaea (Salacia I) 190? 3,500? 136108 Haumea Cubewano 1400 Hiʻiaka (Haumea I) 310 49,500 ± 400 Namaka (Haumea II) 170 39,300 136199 Eris SDO 2,800 Dysnomia (Eris I) 150–250 30,000–36,000 148780 Altjira Cubewano 340? S/2007 (148780) 1 246? 5,800? edit] See also Yarkovsky-O'Keefe-Radzievskii-Paddack effect (YORP effect) References ^ a b Dr. William J. Merline and Maria Martinez (2000-10-26). "Astronomers Image Double Asteroid". SwRI Press Release. http://www.boulder.swri.edu/merline/press/release.txt. Retrieved 2009-10-20.  (mentions both 90 Antiope and 762 Pulcova) ^ a b c d e f Wm. Robert Johnston (2009-10-16). "Asteroids with Satellites". Johnston's Archive. http://www.johnstonsarchive.net/astro/asteroidmoons.html. Retrieved 2009-10-20.  ^ "Satellites and Companions of Minor Planets". IAU / Minor Planet Center. 2009-09-17. http://www.cbat.eps.harvard.edu/minorsats.html. Retrieved 2011-01-08.  ^ "90 Antiope: Raw Keck Image". SWrI Press Release. August 2000. http://www.boulder.swri.edu/merline/press/fig1.html. Retrieved 2009-10-20.  ^ "IAUC 8732: S/2006 (624) 1". http://www.cbat.eps.harvard.edu/iauc/08700/08732.html#Item1. Retrieved 2011-01-08.  (Satellite Discovery) ^ a b Marchis, F.; Baek, M.,; Berthier, J.; Descamps, P.; Emery, J.P.; Macomber, B.; Pollock, J.; Vachier, F. (2008). "Multiple Asteroid Systems: New Techniques to Study New Worlds". Lunar and Planetary Institute. http://www.lpi.usra.edu/meetings/acm2008/pdf/8321.pdf. Retrieved 2009-10-20.  ^ Satellite of Minor Planet 532 Herculina Discovered During Occultation. David W. Dunham, The Minor Planet Bulletin, Volume 6, p.13–14 (December 1978) ADS archive copy ^ "Astronomers Discover Moon Orbiting Asteroid". SwRI. 1998. http://www.boulder.swri.edu/~merline/press_release/. Retrieved 2009-10-21.  (Eugenia AO image) ^ Merline, W. J. (2001). "IAUC 7741: 2001fc; S/2001 (617) 1; C/2001 T1, C/2001 T2". http://www.cbat.eps.harvard.edu/iauc/07700/07741.html.  ^ Chiang, E.; Lithwick, Y.; Buie, M.; Grundy, W.; Holman, M.; A Brief History of Trans-Neptunian Space, to appear in Protostars and Planets V (August 2006) Final preprint on arXiv ^ Daniel W. E. Green (2005-08-11). "IAUC 8582: Sats OF (87)". International Astronomical Union Circular. http://www.cbat.eps.harvard.edu/iauc/08500/08582.html. Retrieved 2011-01-08.  ^ Daniel W. E. Green (2007-03-07). "IAUC 8817: S/2004 (45) 1". International Astronomical Union Circular. http://www.cbat.eps.harvard.edu/iauc/08800/08817.html. Retrieved 2011-01-08.  ^ Franck Marchis (Principal Investigator, SETI Institute, UC Berkeley). "Franck Marchis Web Page". Department of Astronomy (University of California at Berkeley). http://astro.berkeley.edu/~fmarchis/. Retrieved 2009-10-27.  ^ Franck Marchis (Principal Investigator, SETI Institute, UC Berkeley) (2008-09-19). "Two Companions Found Near Dog-Bone Asteroid". SETI Institute. http://www.seti.org/Page.aspx?pid=1182. Retrieved 2009-10-26.  ^ Franck Marchis (2009-08-21). "The discovery of a new triple asteroid – (93) Minerva". Cosmic Diary Blog. http://www.cosmicdiary.org/blogs/nasa/franck_marchis/?p=465. Retrieved 2009-10-27.  ^ a b Noll, Keith S. "Solar System binaries", Asteroids, Comets, Meteors, Proceedings of the 229th Symposium of the IAU, Rio de Janeiro, 2005, Cambridge University Press, 2006., pp. 301–318 Preprint ^ K. Noll, H. Levison W. Grundy, D. Stephens (October 2006). "Discovery of a binary Centaur". Icarus 184.  ^ "T. Michałowski et al. (2004). "Eclipsing binary asteroid 90 Antiope". Astronomy & Astrophysics 423 (3): 1159. Bibcode 2004A&A...423.1159M. doi:10.1051/0004-6361:20040449.  ^ Bieryla, Allyson; Parker, J. W. (12/2006). "Search for Satellites around Ceres". 2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #25.02; Bulletin of the American Astronomical Society 38: 933. Bibcode 2006AAS...209.2502B.  ^ Brown, M. E. et al. (2006). "Satellites of the Largest Kuiper Belt Objects" (PDF). The Astrophysical Journal 639: L43. arXiv:astro-ph/0510029. Bibcode 2006ApJ...639L..43B. doi:10.1086/501524. http://web.gps.caltech.edu/~mbrown/papers/ps/gab.pdf. Retrieved 2011-10-19.  edit ^ Mike Brown. "Dysnomia, the moon of Eris". Caltech. http://www.gps.caltech.edu/~mbrown/planetlila/moon. Retrieved 2009-07-02.  ^ http://www.cbat.eps.harvard.edu/cbet/000800/CBET000860.txt CBET 860 Asteroids with Satellites web page, maintained up to date by W. Robert Johnston; and references therein. (last accessed 13-03-2007) The VOBAD database a web page built and designed by F. Marchis and his collaborators (UC-Berkeley/SETI Institute) which contains the parameters of 169 multiple asteroid systems (last update May 9, 2009) External links Orbits of Binary Asteroids with Adaptive Optics (Franck Marchis) Satellites and Companions of Minor Planets (CBAT) Asteroids with Satellites (Robert Johnston) Wikimedia Foundation. 2010. Игры ⚽ Нужно сделать НИР? Minor planet designation Minor (academic) Look at other dictionaries: Minor planet — Not to be confused with Dwarf planet. A minor planet is an astronomical object in direct orbit around the Sun that is neither a dominant planet nor a comet, and thus includes the dwarf planets. The orbital categories of minor planets are the… …   Wikipedia Minor planet designation — Formal minor planet designations are number–name combinations overseen by the Minor Planet Center, a branch of the IAU. They are used for dwarf planets and small Solar System bodies such as asteroids, but not comets. They are assigned to a body… …   Wikipedia Minor-planet designation — Formal minor planet designations are number name combinations overseen by the Minor Planet Center, a branch of the IAU. They are used for dwarf planets and small Solar System bodies such as asteroids, but not comets. They are assigned to a body… …   Wikipedia Minor Planet Circular — The Minor Planet Circulars (MPCs) is a scientific journal that is generally published on the date of each full moon by the Minor Planet Center. The Circulars contain astrometric observations, orbits and ephemerides of minor planets, comets and… …   Wikipedia Meanings of minor planet names: 15001–16000 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. The list below concerns those minor planets …   Wikipedia Meanings of minor planet names: 3001–3500 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. The list below concerns those minor planets …   Wikipedia Meanings of minor planet names: 12001–13000 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. The list below concerns those minor planets …   Wikipedia Meanings of minor planet names: 38001–39000 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. The list below concerns those minor planets …   Wikipedia Meanings of minor planet names: 66001–67000 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. The list below concerns those minor planets …   Wikipedia Meanings of minor planet names: 5501–6000 — As minor planet discoveries are confirmed, they are given a permanent number by the IAU s Minor Planet Center, and the discoverers can then submit names for them, following the IAU s naming conventions. 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