Trinary_asteroid

Minor-planet moon

Minor-planet moon

Natural satellite of a minor planet

A minor-planet moon is an astronomical object that orbits a minor planet as its natural satellite. As of January 2022, there are 457 minor planets known or suspected to have moons.[1] 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 into their physical properties that are generally not otherwise accessible.[2]

See also: Binary asteroid

Several of the moons are quite large compared to their primaries: 90 Antiope, Mors–Somnus and Sila–Nunam (95%), Patroclus–Menoetius, Altjira and Lempo–Hiisi (90%, with Lempo–Paha at 50%). The largest known minor-planet moon in absolute size is Pluto's largest moon Charon, which itself has about half the diameter of Pluto.

There are also several known ring systems around distant objects (see: Rings of Chariklo and Chiron).

Terminology

See also: Binary asteroid

In addition to the terms satellite and moon, the term "binary" (binary minor planet) is sometimes used for minor planets with moons, and "triple" for minor planets with two moons. If one object is much bigger it can be 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.[2][5]

Discovery milestones

Prior to the era of the Hubble Space Telescope and space probes reaching the outer Solar System, attempts to detect satellites around asteroids were limited to optical observations from Earth. For example, in 1978, stellar occultation observations were claimed as evidence of a satellite for the asteroid 532 Herculina.[6][7] However, later more-detailed imaging by the Hubble Telescope did not reveal a satellite, and the current consensus is that Herculina does not have a significant satellite.[8] There were other similar reports of asteroids having companions (usually referred to as satellites) in the following years. A letter by astronomer Thomas Hamilton in the Sky & Telescope magazine at this time pointed to apparently simultaneous impact craters on Earth (for example, the Clearwater Lakes in Quebec), suggesting that these craters were caused by pairs of gravitationally bound objects.[9]

Also in 1978, Pluto's largest moon Charon was discovered; however, at the time Pluto was still considered to be one of the major planets.

In 1993, the first asteroid moon was confirmed when the Galileo probe discovered the small Dactyl orbiting 243 Ida in the asteroid belt. The second was discovered around 45 Eugenia in 1998.[10] In 2001, 617 Patroclus and its same-sized companion Menoetius became the first known binary asteroids in the Jupiter trojans.[11] The first trans-Neptunian binary after Pluto–Charon, 1998 WW31, was optically resolved in 2002.[12]

Multiple systems

In 2005, the asteroid 87 Sylvia was discovered to have two satellites, making it the first known triple system (also called trinary minor planets).[13] This was followed by the discovery of a second moon orbiting 45 Eugenia.[14] Also in 2005, the dwarf planet Haumea was discovered to have two moons, making it the second trans-Neptunian object after Pluto known to have more than one moon.[15] Additionally, 216 Kleopatra[16] and 93 Minerva[17] were discovered to be trinary asteroids in 2008 and 2009 respectively. Since the first few triple minor planets were discovered, more continue to be discovered at a rate of about one a year. Most recently discovered were two moons orbiting large near-earth asteroid 3122 Florence, bringing the number of known multiple systems in the Solar System up to 16 (including the Pluto and Haumea systems).

The following table lists all satellites of multiple systems, starting with Pluto, which was unnumbered when its first moon was discovered in 1978. The highest known multiplicities are for Pluto (a sextuple system) and 130 Elektra (a quadruple system).

More information Parent body, Designation ...

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 (TNOs), an estimated 11% are thought to be binary or multiple objects, and the majority of the large TNOs have at least one satellite, including all four IAU-listed dwarf planets.

More than 50 binaries are known in each of the main groupings: near-Earth asteroids, belt asteroids, and trans-Neptunian objects, not including numerous claims based solely on light-curve variation.

Two binaries have been found so far among centaurs with semi-major axes smaller than Neptune.[18] Both are double ring systems around 2060 Chiron and 10199 Chariklo, discovered in 1993–2011 and 2013 respectively.

Origin

The origin of minor-planet moons is not currently known with certainty, and a variety of hypotheses exist. One such model is that minor-planet moons are formed from debris knocked off 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 the 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.[18]

Populations and classes

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).[19]

  • 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.
The eight largest TNOs with moons (Pluto, Haumea, Makemake, Eris, Quaoar, Gonggong, Orcus and Salacia), with the Earth to scale. Gonggong is written as its provisional designation, 2007 OR10.
  • 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.
    • Pluto has five known moons. Its largest moon Charon is more than half the size of Pluto itself, and large enough to orbit a point outside Pluto's surface. In fact, each orbits the common barycenter between them, with Pluto's orbit entirely enclosed by Charon's; thus they form a binary system informally referred to as a double dwarf planet. Pluto's four other moons, Nix, Hydra, Kerberos, and Styx, are far smaller and orbit the Pluto–Charon system.
    • Haumea has two moons with radii estimated around 155 km (Hiʻiaka) and 85 km (Namaka).
    • Makemake has one known moon, S/2015 (136472) 1, estimated to be some 160 kilometers (100 mi) in diameter.
    • 47171 Lempo is a unique trans-Neptunian triple system: Lempo and its moon of roughly equal mass, Hiisi, form a close-proximity binary, separated by roughly 867 km. A second moon, Paha, orbits the Lempo–Hiisi binary at about 7411 km.
    • Eris has one known moon, Dysnomia. Its radius, based on its brightness, is estimated to be roughly between 150 and 350 km.[20]

List

As of January 2022, there are 457 minor planets (systems) with 477 known companions.[1] The following table is a listing of the total number of these systems by orbital class:

More information # of Systems, Orbital class ...

Near-Earth objects

This is a list of near-Earth asteroids with companions.[1] Candidate binaries with an unconfirmed status are displayed on a dark background.[22] For an overview, see summary and introduction.

More information System, Primary ...

Mars crossers

This is a list of Mars-crossing asteroids with companions.[1] Candidate binaries with an unconfirmed status are displayed on a dark background.[22] For an overview, see summary and introduction.

More information System, Primary ...

Main-belt asteroids

This is a list of main-belt asteroids with companions.[1] Candidate binaries with an unconfirmed status are displayed on a dark background.[22] For an overview, see summary and introduction.

More information System, Primary ...

The following binaries are double asteroids, with similarly sized components, and a barycenter outside of the larger object.

  1. 90 Antiope — S/2000 (90) 1
  2. 854 Frostia — S/2004 (854) 1
  3. 1313 Berna — S/2004 (1313) 1
  4. 2478 Tokai — S/2007 (2478) 1
  5. 3169 Ostro — S/2005 (3169) 1
  6. 3749 Balam — S/2002 (3749) 1
  7. 3905 Doppler — S/2013 (3905) 1
  8. 4674 Pauling — S/2004 (4674) 1
  9. 4951 Iwamoto — S/2007 (4951) 1
  10. 5674 Wolff — S/2015 (5674) 1
  11. 8474 Rettig — S/2015 (8474) 1
  12. 17246 Christophedumas — S/2004 (17246) 1
  13. (300163) 2006 VW139 — S/2011 (300163) 1

In addition, these bodies might be double asteroids, but due to errors in their size and orbit, it is uncertain.

  1. 809 Lundia — S/2005 (809) 1
  2. 1089 Tama — S/2003 (1089) 1
  3. 1509 Esclangona — S/2003 (1509) 1
  4. 4492 Debussy — S/2004 (4492) 1
  5. 11264 Claudiomaccone — S/2003 (11264) 1
  6. 22899 Alconrad — S/2003 (22899) 1

Jupiter trojans

This is a list of Jupiter trojans with companions.[1] Candidate binaries with an unconfirmed status are displayed on a dark background.[22] For an overview, see summary and introduction.

More information System, Primary ...

Trans-Neptunian objects

This is a list of trans-Neptunian objects with companions.[1] Candidate binaries with an unconfirmed status are displayed on a dark background.[22] This list gives the companion's orbital period (Ps) in days rather than hours. For an overview, see summary and introduction.

More information System, Primary ...

See also

References

  1. [1]
    Johnston, Wm. Robert (23 January 2022). "Asteroids with Satellites". Johnston's Archive. Retrieved 13 February 2022.
  2. [2]
    William J. Merline; Maria Martinez (26 October 2000). "Astronomers Image Double Asteroid". SwRI Press Release. Retrieved 27 November 2018. (mentions both 90 Antiope and 762 Pulcova)
  3. [3]
    "Satellites and Companions of Minor Planets". IAU / Minor Planet Center. 17 September 2009. Retrieved 27 November 2018.
  4. [4]
    "90 Antiope: Raw Keck Image". SWrI Press Release. August 2000. Retrieved 27 November 2018.
  5. [5]
    "IAUC 8732: S/2006 (624) 1". Central Bureau for Astronomical Telegrams. 21 July 2006. Retrieved 26 November 2018. (Satellite Discovery)
  6. [6]
    Dunham, David W. (December 1978). "Satellite of Minor Planet 532 Herculina Discovered During Occultation". The Minor Planet Bulletin. 6: 13–14. Bibcode:1978MPBu....6...13D.
  7. [7]
    Dunham, David W.; Maley, Paul D. (December 1977). "Possible Observation of a Satellite of a Minor Planet". The Minor Planet Bulletin. 5: 16–17. Bibcode:1977MPBu....5...16D.
  8. [8]
    Storrs, Alex; Weiss, Ben; Zellner, Ben; Burleson, Win; Sichitiu, Rukmini; Wells, Eddie; et al. (February 1999). "Imaging Observations of Asteroids with Hubble Space Telescope" (PDF). Icarus. 137 (2): 260–268. Bibcode:1999Icar..137..260S. doi:10.1006/icar.1999.6047. S2CID 274199. Archived from the original (PDF) on 14 June 2018.
  9. [9]
    Hamilton, Thomas Wm. (27 August 2014). Impact Craters of Earth: with Selected Craters Elsewhere. Strategic Book Publishing & Rights Agency. p. 24. ISBN 9781631353536. Retrieved 28 February 2021.
  10. [10]
    "Astronomers Discover Moon Orbiting Asteroid". SwRI. 1998. Retrieved 2 January 2019. (Eugenia AO image)
  11. [11]
    Merline, W. J. (29 October 2001). "IAUC 7741: 2001fc; S/2001 (617) 1; C/2001 T1, C/2001 T2". Central Bureau for Astronomical Telegrams.
  12. [12]
    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
  13. [13]
    Daniel W. E. Green (11 August 2005). "IAUC 8582: Sats OF (87)". Central Bureau for Astronomical Telegrams. Retrieved 8 January 2011.
  14. [14]
    Daniel W. E. Green (7 March 2007). "IAUC 8817: S/2004 (45) 1". Central Bureau for Astronomical Telegrams. Retrieved 8 January 2011.
  15. [15]
    Marchis, Franck. "Franck Marchis Web Page (Principal Investigator, SETI Institute, UC Berkeley)". Department of Astronomy (University of California at Berkeley). Archived from the original on 10 November 2007. Retrieved 27 October 2009.
  16. [16]
    Marchis, Franck (19 September 2008). "Two Companions Found Near Dog-Bone Asteroid". SETI Institute. Archived from the original on 27 September 2011. Retrieved 26 October 2009.
  17. [17]
    Franck Marchis (21 August 2009). "The discovery of a new triple asteroid – (93) Minerva". Cosmic Diary Blog. Archived from the original on 9 June 2012. Retrieved 27 October 2009.
  18. [18]
    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
  19. [19]
    T. Michałowski; et al. (2004). "Eclipsing binary asteroid 90 Antiope". Astronomy & Astrophysics. 423 (3): 1159–1168. Bibcode:2004A&A...423.1159M. doi:10.1051/0004-6361:20040449.
  20. [20]
    Santos-Sanz, P.; et al. (2012). ""TNOs are Cool": A Survey of the Transneptunian Region IV. Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS". Astronomy & Astrophysics. 541: A92. arXiv:1202.1481. Bibcode:2012A&A...541A..92S. doi:10.1051/0004-6361/201118541. S2CID 118600525.
  21. [21]
    Marchis, F.; Baek, M.; Berthier, J.; Descamps, P.; et al. (2008). "Multiple Asteroid Systems: New Techniques to Study New Worlds" (PDF). Lunar and Planetary Institute. Retrieved 20 October 2009.
  22. [22]
    Johnston, Wm. Robert (24 December 2021). "Asteroids/TNOs with Satellites list by type and presumed level of confirmation". Johnston's Archive. Retrieved 13 February 2022.
  23. [23]
    Clark, Stephen (14 June 2022). "Ninth asteroid added to Lucy mission; optimism grows on solar array issue". Spaceflight Now. Retrieved 15 June 2022.
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