Binary asteroid

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Binary asteroid 243 Ida with its small minor-planet moon, Dactyl, as seen by Galileo 243 ida crop.jpg
Binary asteroid 243 Ida with its small minor-planet moon, Dactyl, as seen by Galileo
Binary near-Earth asteroid 65803 Didymos and its moon Dimorphos imaged by the Double Asteroid Redirection Test spacecraft Didymos-Dimorphos true orientation.png
Binary near-Earth asteroid 65803 Didymos and its moon Dimorphos imaged by the Double Asteroid Redirection Test spacecraft

A binary asteroid is a system of two asteroids orbiting their common barycenter. The binary nature of 243 Ida was discovered when the Galileo spacecraft flew by the asteroid in 1993. Since then numerous binary asteroids and several triple asteroids have been detected. [1]

Contents

The mass ratio of the two components – called the "primary" and "secondary" of a binary system – is an important characteristic. Most binary asteroids have a large mass ratio, i.e. a relatively small satellite in orbit around the main component. Systems with a small minor-planet moon – also called "companion" or simply "satellite" – include 87 Sylvia, 107 Camilla, 45 Eugenia, 121 Hermione, 130 Elektra, 22 Kalliope, 283 Emma, 379 Huenna, 243 Ida and 4337 Arecibo (in order of decreasing primary size). Some binary systems have a mass ratio near unity, i.e., two components of similar mass. They include 90 Antiope, 2006 VW139 , 2017 YE5 and 69230 Hermes, with average component diameters of 86, 1.8, 0.9 and 0.8 km, respectively.

In August 2024 Gaia reported 352 new binary asteroid candidates. [2] [3]

Description

Several theories have been posited to explain the formation of binary-asteroid systems. Many systems have significant macro-porosity (a "rubble-pile" interior). The satellites orbiting large main-belt asteroids such as 22 Kalliope, 45 Eugenia or 87 Sylvia may have formed by disruption of a parent body after impact or fission after an oblique impact. Trans-Neptunian binaries may have formed during the formation of the Solar System by mutual capture or three-body interaction. Near-Earth asteroids, which orbit in the inner part of the Solar System, most likely form by spin-up and mass shedding, [4] likely as a result of the YORP effect. Numerical simulations suggest that when solar energy spins a “rubble pile” asteroid to a sufficiently fast rate by the YORP effect, material is thrown from the asteroid's equator. [5] This process also exposes fresh material at the poles of the asteroid. [5] [6]

See also

Related Research Articles

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<span class="mw-page-title-main">Natural satellite</span> Astronomical body that orbits a planet

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<span class="mw-page-title-main">Minor-planet moon</span> 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. Discoveries of minor-planet moons 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.

<span class="mw-page-title-main">90 Antiope</span> Double asteroid system in the outer asteroid belt

90 Antiope is a double asteroid in the outer asteroid belt. It was discovered on October 1, 1866, by Robert Luther. In 2000, it was found to consist of two almost-equally-sized bodies orbiting each other. At average diameters of about 88 km and 84 km, both components are among the 500 largest asteroids. Antiope is a member of the Themis family of asteroids that share similar orbital elements.

<span class="mw-page-title-main">45 Eugenia</span> Asteroid with 2 moons

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<span class="mw-page-title-main">22 Kalliope</span> Main-belt asteroid

22 Kalliope is a large M-type asteroid from the asteroid belt discovered by J. R. Hind on 16 November 1852. It is named after Calliope, the Greek Muse of epic poetry. It is orbited by a small moon named Linus.

<span class="mw-page-title-main">YORP effect</span> Second-order variation on the Yarkovsky effect that changes the rotation rate of a small body

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Jean-Luc Margot is a Belgian-born astronomer and a UCLA professor with expertise in planetary sciences and SETI.

<span class="mw-page-title-main">47171 Lempo</span> System comprising three trans-Neptunian objects

47171 Lempo, or as a binary (47171) Lempo–Hiisi (provisional designation 1999 TC36), is a trans-Neptunian object and trinary system from the Kuiper belt, located in the outermost regions of the Solar System. It was discovered on 1 October 1999, by American astronomers Eric Rubenstein and Louis-Gregory Strolger during an observing run at Kitt Peak National Observatory in Arizona, United States. Rubenstein was searching images taken by Strolger as part of their Nearby Galaxies Supernova Search project. It is classified as a plutino with a 2:3 mean-motion resonance with Neptune and is among the brighter TNOs. It reached perihelion in July 2015. This minor planet was named after Lempo from Finnish mythology.

<span class="mw-page-title-main">3749 Balam</span>

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<span class="mw-page-title-main">Linus (moon)</span> Asteroid moon that orbits 22 Kalliope

Linus, formal designation (22) Kalliope I Linus, is an asteroid moon that orbits the large M-type asteroid 22 Kalliope. It was discovered on August 29, 2001, by astronomers Jean-Luc Margot and Michael E. Brown with the Keck telescope, in Hawaii. Another team also detected the moon with the Canada-France-Hawaii Telescope on September 2, 2001. Both telescopes are on Mauna Kea. It received the provisional designation S/2001 (22) 1, until it was named. The naming proposal appeared in the discovery paper and was approved by the International Astronomical Union in July 2003. Although the naming proposal referred to the mythological Linus, son of the muse Calliope and the inventor of melody and rhythm, the name was also meant to honor Linus Torvalds, inventor of the Linux operating system kernel, and Linus van Pelt, a character in the Peanuts comic strip.

<span class="mw-page-title-main">Contact binary (small Solar System body)</span> Small Solar System body that is composed of two bodies

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<span class="nowrap">(185851) 2000 DP<sub>107</sub></span>

(185851) 2000 DP107 is a sub-kilometer sized asteroid, classified as potentially hazardous asteroid and near-Earth object of the Apollo group that is notable because it provided evidence for binary asteroids in the near-Earth population. The PROCYON probe developed by JAXA and the University of Tokyo was intended to flyby this asteroid before its ion thruster failed and could not be restarted.

4337 Arecibo is a binary asteroid in the outer regions of the asteroid belt, approximately 24 kilometers in diameter. It was discovered on 14 April 1985, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona, in the United States. It was named after the Arecibo Observatory in Puerto Rico. It has a relatively large minor-planet moon that was discovered in stellar occultation observations by David Gault and Peter Nosworthy in May 2021, distinguishing it as the first asteroid moon discovered and confirmed solely using the occultation method.

<span class="mw-page-title-main">Retrograde and prograde motion</span> Relative directions of orbit or rotation

Retrograde motion in astronomy is, in general, orbital or rotational motion of an object in the direction opposite the rotation of its primary, that is, the central object. It may also describe other motions such as precession or nutation of an object's rotational axis. Prograde or direct motion is more normal motion in the same direction as the primary rotates. However, "retrograde" and "prograde" can also refer to an object other than the primary if so described. The direction of rotation is determined by an inertial frame of reference, such as distant fixed stars.

<span class="mw-page-title-main">(35107) 1991 VH</span>

(35107) 1991 VH is a binary near-Earth asteroid and potentially hazardous asteroid of the Apollo group. It was discovered on 9 November 1991, by Australian astronomer Robert McNaught at Siding Spring Observatory. This binary system is composed of a roughly-spheroidal primary body about one kilometre in diameter, and an elongated natural satellite less than half a kilometre in diameter. The 1991 VH system is unusual for its dynamically excited state; the satellite has a tumbling, non-synchronous rotation that chaotically exchanges energy and angular momentum with its precessing, eccentric orbit. This asteroid system was one of the two targets of NASA's upcoming Janus Mayhem mission, until the delay of the rocket launch made both targets inaccessible.

<span class="mw-page-title-main">Satellite system (astronomy)</span> Set of gravitationally bound objects in orbit

A satellite system is a set of gravitationally bound objects in orbit around a planetary mass object or minor planet, or its barycenter. Generally speaking, it is a set of natural satellites (moons), although such systems may also consist of bodies such as circumplanetary disks, ring systems, moonlets, minor-planet moons and artificial satellites any of which may themselves have satellite systems of their own. Some bodies also possess quasi-satellites that have orbits gravitationally influenced by their primary, but are generally not considered to be part of a satellite system. Satellite systems can have complex interactions including magnetic, tidal, atmospheric and orbital interactions such as orbital resonances and libration. Individually major satellite objects are designated in Roman numerals. Satellite systems are referred to either by the possessive adjectives of their primary, or less commonly by the name of their primary. Where only one satellite is known, or it is a binary with a common centre of gravity, it may be referred to using the hyphenated names of the primary and major satellite.

<span class="nowrap">(300163) 2006 VW<sub>139</sub></span> Asteroid in the asteroid belt

(300163) 2006 VW139 (provisional designation 2006 VW139, periodic comet designation 288P/2006 VW139) is a binary active asteroid and main-belt comet from the outer regions of the asteroid belt. The object was discovered by Spacewatch in 2006. Its binary nature was confirmed by the Hubble Space Telescope in September 2016. Both primary and its minor-planet moon are similar in mass and size, making it a true binary system. The components are estimated to measure 1.8 kilometers in diameter, orbiting each other at a wide separation of 104 kilometers every 135 days.

References

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  2. Liberato, L.; Tanga, P.; Mary, D.; Minker, K.; Carry, B.; Spoto, F.; Bartczak, P.; Sicardy, B.; Oszkiewicz, D.; Desmars, J. (August 2024). "Binary asteroid candidates in Gaia DR3 astrometry". Astronomy & Astrophysics. 688: A50. doi:10.1051/0004-6361/202349122. ISSN   0004-6361.
  3. Graham-Shaw, Kate. "These 352 Asteroids Likely Have Cute Little Moonlets". Scientific American. Retrieved 2024-08-14.
  4. Margot, Jean-Luc; et al. (2002). "Binary Asteroids in the Near-Earth Object Population". Science. 296 (5572): 1445–1448. Bibcode:2002Sci...296.1445M. doi:10.1126/science.1072094. PMID   11951001. S2CID   8768432.
  5. 1 2 Walsh, Kevin J.; Richardson, DC; Michel, P (June 2008). "Rotational breakup as the origin of small binary asteroids". Nature. 454 (7201): 188–191. Bibcode:2008Natur.454..188W. doi:10.1038/nature07078. PMID   18615078. S2CID   4418744.
  6. Study Puts Solar Spin on Asteroids, their Moons & Earth Impacts Newswise, Retrieved 14 July 2008.
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