Astronomy:Asteroid belt

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Short description: Region between the orbits of Mars and Jupiter
The asteroids of the inner Solar System and Jupiter: The belt is located between the orbits of Jupiter and Mars.
  Sun
  Jupiter trojans
  Orbits of planets 		  Asteroid belt
  Hilda asteroids (Hildas)
  Near-Earth objects (selection)
By far the largest object within the belt is the dwarf planet Ceres. The total mass of the asteroid belt is significantly less than Pluto's, and roughly twice that of Pluto's moon Charon.

The asteroid belt is a torus-shaped region in the Solar System, centered on the Sun and roughly spanning the space between the orbits of the planets Jupiter and Mars. It contains a great many solid, irregularly shaped bodies called asteroids or minor planets. The identified objects are of many sizes, but much smaller than planets, and, on average, are about one million kilometers (or six hundred thousand miles) apart. This asteroid belt is also called the main asteroid belt or main belt to distinguish it from other asteroid populations in the Solar System.[1]

The asteroid belt is the smallest and innermost known circumstellar disc in the Solar System. Classes of small Solar System bodies in other regions are the near-Earth objects, the centaurs, the Kuiper belt objects, the scattered disc objects, the sednoids, and the Oort cloud objects. About 60% of the main belt mass is contained in the four largest asteroids: Ceres, Vesta, Pallas, and Hygiea. The total mass of the asteroid belt is estimated to be 3% that of the Moon.[2]

Ceres, the only object in the asteroid belt large enough to be a dwarf planet, is about 950 km in diameter, whereas Vesta, Pallas, and Hygiea have mean diameters less than 600 km.[3][4][5][6] The remaining bodies range down to the size of a dust particle. The asteroid material is so thinly distributed that numerous uncrewed spacecraft have traversed it without incident.[7] Nonetheless, collisions between large asteroids occur and can produce an asteroid family, whose members have similar orbital characteristics and compositions. Individual asteroids within the belt are categorized by their spectra, with most falling into three basic groups: carbonaceous (C-type), silicate (S-type), and metal-rich (M-type).

The asteroid belt formed from the primordial solar nebula as a group of planetesimals,[8] the smaller precursors of the protoplanets. Between Mars and Jupiter, however, gravitational perturbations from Jupiter disrupted their accretion into a planet,[8][9] imparting excess kinetic energy which shattered colliding planetesimals and most of the incipient protoplanets. As a result, 99.9% of the asteroid belt's original mass was lost in the first 100 million years of the Solar System's history.[10] Some fragments eventually found their way into the inner Solar System, leading to meteorite impacts with the inner planets. Asteroid orbits continue to be appreciably perturbed whenever their period of revolution about the Sun forms an orbital resonance with Jupiter. At these orbital distances, a Kirkwood gap occurs as they are swept into other orbits.[11]

History of observation

In 1596, Johannes Kepler's sense of proportion for the planetary orbits led him to believe that an invisible planet lay between the orbits of Mars and Jupiter.[12]

In 1596, Johannes Kepler wrote, "Between Mars and Jupiter, I place a planet," in his Mysterium Cosmographicum, stating his prediction that a planet would be found there.[13] While analyzing Tycho Brahe's data, Kepler thought that too large a gap existed between the orbits of Mars and Jupiter to fit Kepler's then-current model of where planetary orbits should be found.[14]

In an anonymous footnote to his 1766 translation of Charles Bonnet's Contemplation de la Nature,[15] the astronomer Johann Daniel Titius of Wittenberg[16][17] noted an apparent pattern in the layout of the planets, now known as the Titius-Bode Law. If one began a numerical sequence at 0, then included 3, 6, 12, 24, 48, etc., doubling each time, and added four to each number and divided by 10, this produced a remarkably close approximation to the radii of the orbits of the known planets as measured in astronomical units, provided one allowed for a "missing planet" (equivalent to 24 in the sequence) between the orbits of Mars (12) and Jupiter (48). In his footnote, Titius declared, "But should the Lord Architect have left that space empty? Not at all."[16] When William Herschel discovered Uranus in 1781, the planet's orbit matched the law almost perfectly, leading some astronomers to conclude that a planet had to be between the orbits of Mars and Jupiter.[18]

Giuseppe Piazzi, discoverer of Ceres, the largest object in the asteroid belt: Ceres was known as a planet, but later reclassified as an asteroid and from 2006 as a dwarf planet.

On January 1, 1801, Giuseppe Piazzi, chairman of astronomy at the University of Palermo, Sicily, found a tiny moving object in an orbit with exactly the radius predicted by this pattern. He dubbed it "Ceres", after the Roman goddess of the harvest and patron of Sicily. Piazzi initially believed it to be a comet, but its lack of a coma suggested it was a planet.[19] Thus, the aforementioned pattern predicted the semimajor axes of all eight planets of the time (Mercury, Venus, Earth, Mars, Ceres, Jupiter, Saturn, and Uranus). Concurrent with the discovery of Ceres, an informal group of 24 astronomers dubbed the "celestial police" was formed under the invitation of Franz Xaver von Zach with the express purpose of finding additional planets; they focused their search for them in the region between Mars and Jupiter where the Titius–Bode law predicted there should be a planet.[20][21]

About 15 months later, Heinrich Olbers, a member of the celestial police, discovered a second object in the same region, Pallas. Unlike the other known planets, Ceres and Pallas remained points of light even under the highest telescope magnifications instead of resolving into discs. Apart from their rapid movement, they appeared indistinguishable from stars.[22]

Accordingly, in 1802, William Herschel suggested they be placed into a separate category, named "asteroids", after the Greek asteroeides, meaning "star-like".[23][24] Upon completing a series of observations of Ceres and Pallas, he concluded,[25]

Neither the appellation of planets nor that of comets can with any propriety of language be given to these two stars ... They resemble small stars so much as hardly to be distinguished from them. From this, their asteroidal appearance, if I take my name, and call them Asteroids; reserving for myself, however, the liberty of changing that name, if another, more expressive of their nature, should occur.

By 1807, further investigation revealed two new objects in the region: Juno and Vesta.[22] The burning of Lilienthal in the Napoleonic wars, where the main body of work had been done,[26] brought this first period of discovery to a close.[22]

Despite Herschel's coinage, for several decades it remained common practice to refer to these objects as planets[15] and to prefix their names with numbers representing their sequence of discovery: 1 Ceres, 2 Pallas, 3 Juno, 4 Vesta. In 1845, though, astronomers detected a fifth object (5 Astraea) and, shortly thereafter, new objects were found at an accelerating rate. Counting them among the planets became increasingly cumbersome. Eventually, they were dropped from the planet list (as first suggested by Alexander von Humboldt in the early 1850s) and Herschel's coinage, "asteroids", gradually came into common use.[15]

The discovery of Neptune in 1846 led to the discrediting of the Titius–Bode law in the eyes of scientists because its orbit was nowhere near the predicted position. To date, no scientific explanation for the law has been given, and astronomers' consensus regards it as a coincidence.[27]

951 Gaspra, the first asteroid imaged by a spacecraft, as viewed during Galileo's 1991 flyby; colors are exaggerated

The expression "asteroid belt" came into use in the early 1850s, although pinpointing who coined the term is difficult. The first English use seems to be in the 1850 translation (by Elise Otté) of Alexander von Humboldt's Cosmos:[28] "[...] and the regular appearance, about the 13th of November and the 11th of August, of shooting stars, which probably form part of a belt of asteroids intersecting the Earth's orbit and moving with planetary velocity". Another early appearance occurred in Robert James Mann's A Guide to the Knowledge of the Heavens:[29] "The orbits of the asteroids are placed in a wide belt of space, extending between the extremes of [...]". The American astronomer Benjamin Peirce seems to have adopted that terminology and to have been one of its promoters.[30]

Over 100 asteroids had been located by mid-1868, and in 1891, the introduction of astrophotography by Max Wolf accelerated the rate of discovery still further.[31] A total of 1,000 asteroids had been found by 1921,[32] 10,000 by 1981,[33] and 100,000 by 2000.[34] Modern asteroid survey systems now use automated means to locate new minor planets in ever-increasing numbers.

On 22 January 2014, European Space Agency (ESA) scientists reported the detection, for the first definitive time, of water vapor on Ceres, the largest object in the asteroid belt.[35] The detection was made by using the far-infrared abilities of the Herschel Space Observatory.[36] The finding was unexpected because comets, not asteroids, are typically considered to "sprout jets and plumes". According to one of the scientists, "The lines are becoming more and more blurred between comets and asteroids".[36]

Origin

The asteroid belt showing the orbital inclinations versus distances from the Sun, with asteroids in the core region of the asteroid belt in red and other asteroids in blue

Formation

In 1802, shortly after discovering Pallas, Olbers suggested to Herschel that Ceres and Pallas were fragments of a much larger planet that once occupied the Mars–Jupiter region, with this planet having suffered an internal explosion or a cometary impact many million years before,[37] while Odesan astronomer K. N. Savchenko suggested that Ceres, Pallas, Juno, and Vesta were escaped moons rather than fragments of the exploded planet.[38] The large amount of energy required to destroy a planet, combined with the belt's low combined mass, which is only about 4% of the mass of Earth's Moon,[3] does not support these hypotheses. Further, the significant chemical differences between the asteroids become difficult to explain if they come from the same planet.[39]

A modern hypothesis for the asteroid belt's creation relates to how, in general for the Solar System, planetary formation is thought to have occurred via a process comparable to the long-standing nebular hypothesis; a cloud of interstellar dust and gas collapsed under the influence of gravity to form a rotating disc of material that then conglomerated to form the Sun and planets.[40] During the first few million years of the Solar System's history, an accretion process of sticky collisions caused the clumping of small particles, which gradually increased in size. Once the clumps reached sufficient mass, they could draw in other bodies through gravitational attraction and become planetesimals. This gravitational accretion led to the formation of the planets.[41]

Planetesimals within the region that would become the asteroid belt were strongly perturbed by Jupiter's gravity.[42] Orbital resonances occurred where the orbital period of an object in the belt formed an integer fraction of the orbital period of Jupiter, perturbing the object into a different orbit; the region lying between the orbits of Mars and Jupiter contains many such orbital resonances. As Jupiter migrated inward following its formation, these resonances would have swept across the asteroid belt, dynamically exciting the region's population and increasing their velocities relative to each other.[43] In regions where the average velocity of the collisions was too high, the shattering of planetesimals tended to dominate over accretion,[44] preventing the formation of a planet. Instead, they continued to orbit the Sun as before, occasionally colliding.[42]

During the early history of the Solar System, the asteroids melted to some degree, allowing elements within them to be partially or completely differentiated by mass. Some of the progenitor bodies may even have undergone periods of explosive volcanism and formed magma oceans. Because of the relatively small size of the bodies, though, the period of melting was necessarily brief compared to the much larger planets, and had generally ended about 4.5 billion years ago, in the first tens of millions of years of formation.[45] In August 2007, a study of zircon crystals in an Antarctic meteorite believed to have originated from Vesta suggested that it, and by extension the rest of the asteroid belt, had formed rather quickly, within 10 million years of the Solar System's origin.[46]

Evolution

Large main belt asteroid 4 Vesta

The asteroids are not pristine samples of the primordial Solar System. They have undergone considerable evolution since their formation, including internal heating (in the first few tens of millions of years), surface melting from impacts, space weathering from radiation, and bombardment by micrometeorites.[47][48][49][50] Although some scientists refer to the asteroids as residual planetesimals,[51] other scientists consider them distinct.[52]

The current asteroid belt is believed to contain only a small fraction of the mass of the primordial belt. Computer simulations suggest that the original asteroid belt may have contained mass equivalent to the Earth's.[53] Primarily because of gravitational perturbations, most of the material was ejected from the belt within about 1 million years of formation, leaving behind less than 0.1% of the original mass.[42] Since its formation, the size distribution of the asteroid belt has remained relatively stable; no significant increase or decrease in the typical dimensions of the main-belt asteroids has occurred.[54]

The 4:1 orbital resonance with Jupiter, at a radius 2.06 astronomical units (AUs), can be considered the inner boundary of the asteroid belt. Perturbations by Jupiter send bodies straying there into unstable orbits. Most bodies formed within the radius of this gap were swept up by Mars (which has an aphelion at 1.67 AU) or ejected by its gravitational perturbations in the early history of the Solar System.[55] The Hungaria asteroids lie closer to the Sun than the 4:1 resonance, but are protected from disruption by their high inclination.[56]

When the asteroid belt was first formed, the temperatures at a distance of 2.7 AU from the Sun formed a "snow line" below the freezing point of water. Planetesimals formed beyond this radius were able to accumulate ice.[57][58] In 2006, a population of comets had been discovered within the asteroid belt beyond the snow line, which may have provided a source of water for Earth's oceans. According to some models, outgassing of water during the Earth's formative period was insufficient to form the oceans, requiring an external source such as a cometary bombardment.[59]

The outer asteroid belt appears to include a few objects that may have arrived there during the last few hundred years, the list includes (457175) 2008 GO98 also known as 362P.[60]

Characteristics

Size distribution of asteroids in the main belt[61]

Contrary to popular imagery, the asteroid belt is mostly empty. The asteroids are spread over such a large volume that reaching an asteroid without aiming carefully would be improbable. Nonetheless, hundreds of thousands of asteroids are currently known, and the total number ranges in the millions or more, depending on the lower size cutoff. Over 200 asteroids are known to be larger than 100 km,[62] and a survey in the infrared wavelengths has shown that the asteroid belt has between 700,000 and 1.7 million asteroids with a diameter of 1 km or more.[63]

The number of asteroids in the main belt steadily increases with decreasing size. Although the size distribution generally follows a power law, there are 'bumps' in the curve at about 5 km and 100 km, where more asteroids than expected from such a curve are found. Most asteroids larger than approximately 120 km in diameter are primordial, having survived from the accretion epoch, whereas most smaller asteroids are products of fragmentation of primordial asteroids. The primordial population of the main belt was probably 200 times what it is today.[64][65]

The absolute magnitudes of most of the known asteroids are between 11 and 19, with the median at about 16.[66] On average the distance between the asteroids is about 965,600 km (600,000 mi),[67][68] although this varies among asteroid families and smaller undetected asteroids might be even closer. The total mass of the asteroid belt is estimated to be 2.39×1021 kg, which is just 3% of the mass of the Moon.[2] The four largest objects, Ceres, Vesta, Pallas, and Hygiea, contain an estimated 62% of the belt's total mass, with 39% accounted for by Ceres alone.[69][5]

Composition

Main page: Astronomy:Asteroid spectral types
Distribution of asteroid spectral types by distance from the Sun[70]

The present day belt consists primarily of three categories of asteroids: C-type carbonaceous asteroids, S-type silicate asteroids, and a hybrid group of X-type asteroids. The latter have featureless spectra, but they can be divided into three groups based on reflectivity, yielding the M-type metallic, P-type primitive, and E-type enstatite asteroids. Additional types have been found that do not fit within these primary classes. There is a compositional trend of asteroid types by increasing distance from the Sun, in the order of S, C, P, and the spectrally-featureless D-types.[71]

Fragment of the Allende meteorite, a carbonaceous chondrite that fell to Earth in Mexico in 1969

Carbonaceous asteroids, as their name suggests, are carbon-rich. They dominate the asteroid belt's outer regions,[72] and are rare in the inner belt.[71] Together they comprise over 75% of the visible asteroids. They are redder in hue than the other asteroids and have a very low albedo. Their surface compositions are similar to carbonaceous chondrite meteorites. Chemically, their spectra match the primordial composition of the early Solar System, with the lighter elements and volatiles removed.[73]

S-type (silicate-rich) asteroids are more common toward the inner region of the belt, within 2.5 AU of the Sun.[72][74] The spectra of their surfaces reveal the presence of silicates and some metal, but no significant carbonaceous compounds. This indicates that their materials have been significantly modified from their primordial composition, probably through melting and reformation. They have a relatively high albedo and form about 17% of the total asteroid population.[73]

M-type (metal-rich) asteroids are typically found in the middle of the main belt, and they make up much of the remainder of the total population.[73] Their spectra resemble that of iron-nickel. Some are believed to have formed from the metallic cores of differentiated progenitor bodies that were disrupted through collision. However, some silicate compounds also can produce a similar appearance. For example, the large M-type asteroid 22 Kalliope does not appear to be primarily composed of metal.[75] Within the asteroid belt, the number distribution of M-type asteroids peaks at a semimajor axis of about 2.7 AU.[76] Whether all M-types are compositionally similar, or whether it is a label for several varieties which do not fit neatly into the main C and S classes is not yet clear.[77]

One mystery is the relative rarity of V-type (Vestoid) or basaltic asteroids in the asteroid belt.[78] Theories of asteroid formation predict that objects the size of Vesta or larger should form crusts and mantles, which would be composed mainly of basaltic rock, resulting in more than half of all asteroids being composed either of basalt or olivine. However, observations suggest that 99% of the predicted basaltic material is missing.[79] Until 2001, most basaltic bodies discovered in the asteroid belt were believed to originate from the asteroid Vesta (hence their name V-type), but the discovery of the asteroid 1459 Magnya revealed a slightly different chemical composition from the other basaltic asteroids discovered until then, suggesting a different origin.[79] This hypothesis was reinforced by the further discovery in 2007 of two asteroids in the outer belt, 7472 Kumakiri and (10537) 1991 RY16, with a differing basaltic composition that could not have originated from Vesta. These latter two are the only V-type asteroids discovered in the outer belt to date.[78]

Hubble views the multi-tailed cometary asteroid P/2013 P5.[80]

The temperature of the asteroid belt varies with the distance from the Sun. For dust particles within the belt, typical temperatures range from 200 K (−73 °C) at 2.2 AU down to 165 K (−108 °C) at 3.2 AU.[81] However, due to rotation, the surface temperature of an asteroid can vary considerably as the sides are alternately exposed to solar radiation and then to the stellar background.

Main-belt comets

Main page: Astronomy:Main-belt comet

Several otherwise unremarkable bodies in the outer belt show cometary activity. Because their orbits cannot be explained through the capture of classical comets, many of the outer asteroids are thought to be icy, with the ice occasionally exposed to sublimation through small impacts. Main-belt comets may have been a major source of the Earth's oceans because the deuterium-hydrogen ratio is too low for classical comets to have been the principal source.[82]

Orbits

The asteroid belt (showing eccentricities), with the asteroid belt in red and blue ("core" region in red)

Most asteroids within the asteroid belt have orbital eccentricities of less than 0.4, and an inclination of less than 30°. The orbital distribution of the asteroids reaches a maximum at an eccentricity around 0.07 and an inclination below 4°.[66] Thus, although a typical asteroid has a relatively circular orbit and lies near the plane of the ecliptic, some asteroid orbits can be highly eccentric or travel well outside the ecliptic plane.

Sometimes, the term "main belt" is used to refer only to the more compact "core" region where the greatest concentration of bodies is found. This lies between the strong 4:1 and 2:1 Kirkwood gaps at 2.06 and 3.27 AU, and at orbital eccentricities less than roughly 0.33, along with orbital inclinations below about 20°. (As of 2006), this "core" region contained 93% of all discovered and numbered minor planets within the Solar System.[83] The JPL Small-Body Database lists over 1 million known main-belt asteroids.[84]

Kirkwood gaps

Main page: Astronomy:Kirkwood gap
Number of asteroids in the main belt as a function of their semimajor axis (a). The dashed lines indicate Kirkwood gaps, while colors designate the following zones:
  I: inner main-belt (a < 2.5 AU)
  II: middle main-belt (2.5 AU < a < 2.82 AU)
  III: outer main-belt (a > 2.82 AU)

The semimajor axis of an asteroid is used to describe the dimensions of its orbit around the Sun, and its value determines the minor planet's orbital period. In 1866, Daniel Kirkwood announced the discovery of gaps in the distances of these bodies' orbits from the Sun. They were located in positions where their period of revolution about the Sun was an integer fraction of Jupiter's orbital period. Kirkwood proposed that the gravitational perturbations of the planet led to the removal of asteroids from these orbits.[85]

When the mean orbital period of an asteroid is an integer fraction of the orbital period of Jupiter, a mean-motion resonance with the gas giant is created that is sufficient to perturb an asteroid to new orbital elements. Primordial asteroids entered these gaps because of the migration of Jupiter's orbit.[86] Subsequently, asteroids primarily migrate into these gap orbits due to the Yarkovsky effect,[71] but may also enter because of perturbations or collisions. After entering, an asteroid is gradually nudged into a different, random orbit with a larger or smaller semimajor axis.

Collisions

The zodiacal light, parts of which are reflected by interplanetary dust, which in turn originates in part from collisions of asteroids.

The high population of the asteroid belt makes for a very active environment, where collisions between asteroids occur frequently (on astronomical time scales). Impact events between main-belt bodies with a mean radius of 10 km are expected to occur about once every 10 million years.[87] A collision may fragment an asteroid into numerous smaller pieces (leading to the formation of a new asteroid family).[88] Conversely, collisions that occur at low relative speeds may also join two asteroids. After more than 4 billion years of such processes, the members of the asteroid belt now bear little resemblance to the original population.

Evidence suggests that most main belt asteroids between 200 m and 10 km in diameter are rubble piles formed by collisions. These bodies consist of a multitude of irregular objects that are mostly bound together by self-gravity, resulting in significant amounts of internal porosity.[89] Along with the asteroid bodies, the asteroid belt also contains bands of dust with particle radii of up to a few hundred micrometres. This fine material is produced, at least in part, from collisions between asteroids, and by the impact of micrometeorites upon the asteroids. Due to the Poynting–Robertson effect, the pressure of solar radiation causes this dust to slowly spiral inward toward the Sun.[90]

The combination of this fine asteroid dust, as well as ejected cometary material, produces the zodiacal light. This faint auroral glow can be viewed at night extending from the direction of the Sun along the plane of the ecliptic. Asteroid particles that produce visible zodiacal light average about 40 μm in radius. The typical lifetimes of main-belt zodiacal cloud particles are about 700,000 years. Thus, to maintain the bands of dust, new particles must be steadily produced within the asteroid belt.[90] It was once thought that collisions of asteroids form a major component of the zodiacal light. However, computer simulations by Nesvorný and colleagues attributed 85 percent of the zodiacal-light dust to fragmentations of Jupiter-family comets, rather than to comets and collisions between asteroids in the asteroid belt. At most 10 percent of the dust is attributed to the asteroid belt.[91]

Meteorites

Some of the debris from collisions can form meteoroids that enter the Earth's atmosphere.[92] Of the 50,000 meteorites found on Earth to date, 99.8 percent are believed to have originated in the asteroid belt.[93]

Families and groups

Main page: Astronomy:Asteroid family
This plot of orbital inclination (ip) versus eccentricity (ep) for the numbered main-belt asteroids clearly shows clumpings representing asteroid families.
Overview of the Inner Solar System asteroids up to the Jovian System
Linear overview of the Inner Solar System bodies

In 1918, the Japanese astronomer Kiyotsugu Hirayama noticed that the orbits of some of the asteroids had similar parameters, forming families or groups.[94]

Approximately one-third of the asteroids in the asteroid belt are members of an asteroid family. These share similar orbital elements, such as semi-major axis, eccentricity, and orbital inclination as well as similar spectral features, all of which indicate a common origin in the breakup of a larger body. Graphical displays of these element pairs, for members of the asteroid belt, show concentrations indicating the presence of an asteroid family. There are about 20 to 30 associations that are almost certainly asteroid families. Additional groupings have been found that are less certain. Asteroid families can be confirmed when the members display similar spectral features.[95] Smaller associations of asteroids are called groups or clusters.

Some of the most prominent families in the asteroid belt (in order of increasing semi-major axes) are the Flora, Eunomia, Koronis, Eos, and Themis families.[76] The Flora family, one of the largest with more than 800 known members, may have formed from a collision less than 1 billion years ago.[96] The largest asteroid to be a true member of a family is 4 Vesta. (This is in contrast to an interloper, in the case of Ceres with the Gefion family.) The Vesta family is believed to have formed as the result of a crater-forming impact on Vesta. Likewise, the HED meteorites may also have originated from Vesta as a result of this collision.[97]

Three prominent bands of dust have been found within the asteroid belt. These have similar orbital inclinations as the Eos, Koronis, and Themis asteroid families, and so are possibly associated with those groupings.[98]

The main belt evolution after the Late Heavy Bombardment was very likely affected by the passages of large Centaurs and trans-Neptunian objects (TNOs). Centaurs and TNOs that reach the inner Solar System can modify the orbits of main belt asteroids, though only if their mass is of the order of 10−9 M☉ for single encounters or, one order less in case of multiple close encounters. However, Centaurs and TNOs are unlikely to have significantly dispersed young asteroid families in the main belt, although they can have perturbed some old asteroid families. Current main belt asteroids that originated as Centaurs or trans-Neptunian objects may lie in the outer belt with short lifetime of less than 4 million years, most likely orbiting between 2.8 and 3.2 AU at larger eccentricities than typical of main belt asteroids.[99]

Periphery

Skirting the inner edge of the belt (ranging between 1.78 and 2.0 AU, with a mean semi-major axis of 1.9 AU) is the Hungaria family of minor planets. They are named after the main member, 434 Hungaria; the group contains at least 52 named asteroids. The Hungaria group is separated from the main body by the 4:1 Kirkwood gap and their orbits have a high inclination. Some members belong to the Mars-crossing category of asteroids, and gravitational perturbations by Mars are likely a factor in reducing the total population of this group.[56]

Another high-inclination group in the inner part of the asteroid belt is the Phocaea family. These are composed primarily of S-type asteroids, whereas the neighboring Hungaria family includes some E-types.[100] The Phocaea family orbit between 2.25 and 2.5 AU from the Sun.[101]

Skirting the outer edge of the asteroid belt is the Cybele group, orbiting between 3.3 and 3.5 AU. These have a 7:4 orbital resonance with Jupiter. The Hilda family orbit between 3.5 and 4.2 AU with relatively circular orbits and a stable 3:2 orbital resonance with Jupiter. There are few asteroids beyond 4.2 AU, until Jupiter's orbit. At the latter the two families of Trojan asteroids can be found, which, at least for objects larger than 1 km, are approximately as numerous as the asteroids of the asteroid belt.[102]

New families

Some asteroid families have formed recently, in astronomical terms. The Karin family apparently formed about 5.7 million years ago from a collision with a progenitor asteroid 33 km in radius.[103] The Veritas family formed about 8.3 million years ago; evidence includes interplanetary dust recovered from ocean sediment.[104]

More recently, the Datura cluster appears to have formed about 530,000 years ago from a collision with a main-belt asteroid. The age estimate is based on the probability of the members having their current orbits, rather than from any physical evidence. However, this cluster may have been a source for some zodiacal dust material.[105][106] Other recent cluster formations, such as the Iannini cluster (c. 1–5 million years ago), may have provided additional sources of this asteroid dust.[107]

Exploration

Artist's concept of the Dawn spacecraft with Vesta and Ceres

The first spacecraft to traverse the asteroid belt was Pioneer 10, which entered the region on 16 July 1972. At the time there was some concern that the debris in the belt would pose a hazard to the spacecraft, but it has since been safely traversed by multiple spacecraft without incident. Pioneer 11, Voyagers 1 and 2 and Ulysses passed through the belt without imaging any asteroids. Cassini measured plasma and fine dust grains while traversing the belt in 2000.[108] On its way to Jupiter, Juno traversed the asteroid belt without collecting science data.[109] Due to the low density of materials within the belt, the odds of a probe running into an asteroid are estimated at less than 1 in 1 billion.[110]

Most main belt asteroids imaged to date have come from brief flyby opportunities by probes headed for other targets. Only the Dawn mission has studied main belt asteroids for a protracted period in orbit. The Galileo spacecraft imaged 951 Gaspra in 1991 and 243 Ida in 1993, then NEAR imaged 253 Mathilde in 1997 and landed on near–Earth asteroid 433 Eros in February 2001. Cassini imaged 2685 Masursky in 2000, Stardust imaged 5535 Annefrank in 2002, New Horizons imaged 132524 APL in 2006, and Rosetta imaged 2867 Šteins in September 2008 and 21 Lutetia in July 2010. Dawn orbited Vesta between July 2011 and September 2012 and has orbited Ceres since March 2015.[111]

The Lucy space probe made a flyby of 152830 Dinkinesh in 2023, on its way to the Jupiter Trojans.[112] ESA's JUICE mission will pass through the asteroid belt twice, with a proposed flyby of the asteroid 223 Rosa in 2029.[113] The Psyche spacecraft is a NASA mission to the large M-type asteroid 16 Psyche.[114]

See also

References

  1. ↑ Williams, Matt (2015-08-23). "What is the Asteroid Belt?". Universe Today. http://www.universetoday.com/32856/asteroid-belt/. 
  2. ↑ 2.0 2.1 Pitjeva, E. V. (2018). "Masses of the Main Asteroid Belt and the Kuiper Belt from the Motions of Planets and Spacecraft". Solar System Research 44 (8–9): 554–566. doi:10.1134/S1063773718090050. Bibcode: 2018AstL...44..554P. 
  3. ↑ 3.0 3.1 Krasinsky, G. A.; Pitjeva, E. V.; Vasilyev, M. V.; Yagudina, E. I. (July 2002). "Hidden Mass in the Asteroid Belt". Icarus 158 (1): 98–105. doi:10.1006/icar.2002.6837. Bibcode: 2002Icar..158...98K. 
  4. ↑ Pitjeva, E. V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants". Solar System Research 39 (3): 176–186. doi:10.1007/s11208-005-0033-2. Bibcode: 2005SoSyR..39..176P. http://iau-comm4.jpl.nasa.gov/EPM2004.pdf. 
  5. ↑ 5.0 5.1 For recent estimates of the masses of Ceres, Vesta, Pallas and Hygiea, see the references in the infoboxes of their respective articles.
  6. ↑ Yeomans, Donald K. (July 13, 2006). "JPL Small-Body Database Browser". NASA JPL. http://ssd.jpl.nasa.gov/sbdb.cgi. 
  7. ↑ Koberlein, Brian (2014-03-12). "Why the Asteroid Belt Doesn't Threaten Spacecraft". Universe Today. http://www.universetoday.com/110276/why-the-asteroid-belt-doesnt-threaten-spacecraft/. 
  8. ↑ 8.0 8.1 "How Did The Asteroid Belt Form? Was There A Planet There?". CosmosUp. 2016-01-17. http://www.cosmosup.com/how-did-the-asteroid-belt-form/. 
  9. ↑ Redd, Nola Taylor (2012-06-11). "Asteroid Belt: Facts & Information". Space.com. http://www.space.com/16105-asteroid-belt.html. 
  10. ↑ Beatty, Kelly (March 10, 2009). "Sculpting the Asteroid Belt". Sky & Telescope. http://www.skyandtelescope.com/astronomy-news/sculpting-the-asteroid-belt/. 
  11. ↑ Delgrande, J. J.; Soanes, S. V. (1943). "Kirkwood's Gap in the Asteroid Orbits". Journal of the Royal Astronomical Society of Canada 37: 187. Bibcode: 1943JRASC..37..187D. 
  12. ↑ Cunningham, Clifford J. (September 2022). "The origins and legacy of 'Kepler's Gap'". Journal of Astronomical History and Heritage 25 (3): 439–456. doi:10.3724/SP.J.1440-2807.2022.03.02. Bibcode: 2022JAHH...25..439C. 
  13. ↑ Davis, Phil; Dunford, Bill; Boeck, Moore. "Dawn: Between Jupiter and Mars [sic, I Place a Planet"]. NASA. https://dawn.jpl.nasa.gov/DawnClassrooms/1_hist_dawn/history_discovery/Exploration/fb_jupiter_mars.pdf. 
  14. ↑ Russell, Christopher; Raymond, Carol, eds (2012). The Dawn Mission to Minor Planets 4 Vesta and 1 Ceres. Springer Science+Business Media. p. 5. ISBN 978-1-4614-4902-7. https://books.google.com/books?id=9TMcWJwAyFkC&pg=PA5. 
  15. ↑ 15.0 15.1 15.2 Hilton, J. (2001). "When Did the Asteroids Become Minor Planets?". US Naval Observatory (USNO). http://www.usno.navy.mil/USNO/astronomical-applications/astronomical-information-center/minor-planets. 
  16. ↑ 16.0 16.1 "Dawn: A Journey to the Beginning of the Solar System". Space Physics Center: UCLA. 2005. http://www-ssc.igpp.ucla.edu/dawn/background.html. 
  17. ↑ Hoskin, Michael. "Bode's Law and the Discovery of Ceres". Churchill College, Cambridge. http://www.astropa.unipa.it/versione_inglese/Hystory/BODE%27S_LAW.htm. 
  18. ↑ Nieto, Michael Martin (2014). The Titius-Bode Law of Planetary Distances, Its History and Theory. Elsevier Science. p. 17. ISBN 978-1-4831-5936-2. https://books.google.com/books?id=NneoBQAAQBAJ&pg=PA17. 
  19. ↑ "Call the police! The story behind the discovery of the asteroids". Astronomy Now (June 2007): 60–61. 
  20. ↑ Winterburn, Emily (10 March 2021). "Discovering asteroid Vesta: the story of the Celestial Police". BBC. https://www.skyatnightmagazine.com/space-science/asteroid-vesta-discovery-celestial-police/. 
  21. ↑ McWilliams, Brendan (31 July 2001). "Fruitless search of the Celestial Police". Irish Times. https://www.irishtimes.com/news/fruitless-search-of-the-celestial-police-1.320465. 
  22. ↑ 22.0 22.1 22.2 Staff (2002). "Astronomical Serendipity". NASA JPL. http://dawn.jpl.nasa.gov/DawnCommunity/flashbacks/fb_06.asp. 
  23. ↑ Harper, Douglas (2010). "Asteroid". Online Etymology Dictionary. Etymology Online. http://www.etymonline.com/index.php?search=asteroid&searchmode=none. 
  24. ↑ DeForest, Jessica (2000). "Greek and Latin Roots". Michigan State University. http://www.msu.edu/~defores1/gre/roots/gre_rts_afx2.htm. 
  25. ↑ Cunningham, Clifford (1984). "William Herschel and the First Two Asteroids". The Minor Planet Bulletin (Dance Hall Observatory, Ontario) 11: 3. Bibcode: 1984MPBu...11....3C. 
  26. ↑ Elkins-Tanton, Linda T. (2011). Asteroids, Meteorites, and Comets (Revised ed.). New York: Facts on File. ISBN 978-0-8160-7696-3. OCLC 1054369860. 
  27. ↑ "Is it a coincidence that most of the planets fall within the Titius-Bode law's boundaries?". astronomy.com. http://www.astronomy.com/magazine/ask-astro/2006/10/is-it-a-coincidence-that-most-of-the-planets-fall-within-the-titius-bode-laws-boundaries. 
  28. ↑ von Humboldt, Alexander (1850). Cosmos: A Sketch of a Physical Description of the Universe. 1. New York: Harper & Brothers. p. 44. ISBN 978-0-8018-5503-0. 
  29. ↑ Mann, Robert James (1852). A Guide to the Knowledge of the Heavens. Jarrold. p. 171.  and 1853, p. 216
  30. ↑ "Further Investigation relative to the form, the magnitude, the mass, and the orbit of the Asteroid Planets". The Edinburgh New Philosophical Journal 5: 191. January–April 1857. https://books.google.com/books?id=hhQAAAAAMAAJ&pg=PA191. : "[Professor Peirce] then observed that the analogy between the ring of Saturn and the belt of the asteroids was worthy of notice."
  31. ↑ Hughes, David W. (2007). "A Brief History of Asteroid Spotting". BBC. http://www.open2.net/sciencetechnologynature/planetsbeyond/asteroids/history.html. 
  32. ↑ Moore, Patrick; Rees, Robin (2011). Patrick Moore's Data Book of Astronomy (2nd ed.). Cambridge University Press. p. 156. ISBN 978-0-521-89935-2. 
  33. ↑ Manley, Scott (August 25, 2010). Asteroid Discovery from 1980 to 2010. YouTube. Archived from the original on 2021-10-30. Retrieved 2011-04-15.
  34. ↑ "MPC Archive Statistics". IAU Minor Planet Center. http://www.minorplanetcenter.org/iau/lists/ArchiveStatistics.html. 
  35. ↑ Küppers, Michael; O'Rourke, Laurence; Bockelée-Morvan, Dominique; Zakharov, Vladimir; Lee, Seungwon; von Allmen, Paul; Carry, Benoît; Teyssier, David et al. (2014). "Localized sources of water vapour on the dwarf planet (1) Ceres". Nature 505 (7484): 525–527. doi:10.1038/nature12918. ISSN 0028-0836. PMID 24451541. Bibcode: 2014Natur.505..525K. 
  36. ↑ 36.0 36.1 Harrington, J. D. (22 January 2014). "Herschel Telescope Detects Water on Dwarf Planet – Release 14-021". NASA. http://www.nasa.gov/press/2014/january/herschel-telescope-detects-water-on-dwarf-planet. 
  37. ↑ "A Brief History of Asteroid Spotting". Open2.net. http://www.open2.net/sciencetechnologynature/planetsbeyond/asteroids/history.html. 
  38. ↑ Bronshten, V. A. (1972). "Origin of the Asteroids". NASA. https://archive.org/details/nasa_techdoc_19720017206. 
  39. ↑ Masetti, M.; Mukai, K. (December 1, 2005). "Origin of the Asteroid Belt". NASA Goddard Spaceflight Center. http://imagine.gsfc.nasa.gov/docs/ask_astro/answers/980810a.html. 
  40. ↑ Watanabe, Susan (July 20, 2001). "Mysteries of the Solar Nebula". NASA. http://www.jpl.nasa.gov/news/features.cfm?feature=520. 
  41. ↑ Chambers, John E. (July 2004). "Planetary accretion in the inner Solar System". Earth and Planetary Science Letters 233 (3–4): 241–252. doi:10.1016/j.epsl.2004.04.031. Bibcode: 2004E&PSL.223..241C. 
  42. ↑ 42.0 42.1 42.2 Petit, J.-M.; Morbidelli, A.; Chambers, J. (2001). "The Primordial Excitation and Clearing of the Asteroid Belt". Icarus 153 (2): 338–347. doi:10.1006/icar.2001.6702. Bibcode: 2001Icar..153..338P. http://www.gps.caltech.edu/classes/ge133/reading/asteroids.pdf. Retrieved 2007-03-22. 
  43. ↑ Scott, E. R. D. (March 13–17, 2006). "Constraints on Jupiter's Age and Formation Mechanism and the Nebula Lifetime from Chondrites and Asteroids". League City, Texas: Lunar and Planetary Society. Bibcode: 2006LPI....37.2367S. 
  44. ↑ Edgar, R.; Artymowicz, P. (2004). "Pumping of a Planetesimal Disc by a Rapidly Migrating Planet". Monthly Notices of the Royal Astronomical Society 354 (3): 769–772. doi:10.1111/j.1365-2966.2004.08238.x. Bibcode: 2004MNRAS.354..769E. 
  45. ↑ Taylor, G. J.; Keil, K.; McCoy, T.; Haack, H.; Scott, E. R. D. (1993). "Asteroid differentiation – Pyroclastic volcanism to magma oceans". Meteoritics 28 (1): 34–52. doi:10.1111/j.1945-5100.1993.tb00247.x. Bibcode: 1993Metic..28...34T. 
  46. ↑ Kelly, Karen (2007). "U of T researchers discover clues to early solar system". University of Toronto. http://webapps.utsc.utoronto.ca/ose/story.php?id=665. 
  47. ↑ Clark, B. E.; Hapke, B.; Pieters, C.; Britt, D. (2002). "Asteroid Space Weathering and Regolith Evolution". Asteroids III. University of Arizona. p. 585. doi:10.2307/j.ctv1v7zdn4.44. Bibcode: 2002aste.book..585C. 
  48. ↑ Gaffey, Michael J. (1996). "The Spectral and Physical Properties of Metal in Meteorite Assemblages: Implications for Asteroid Surface Materials". Icarus 66 (3): 468–486. doi:10.1016/0019-1035(86)90086-2. ISSN 0019-1035. Bibcode: 1986Icar...66..468G. 
  49. ↑ Keil, K. (2000). "Thermal alteration of asteroids: evidence from meteorites". Planetary and Space Science. http://www.ingentaconnect.com/content/els/00320633/2000/00000048/00000010/art00054. 
  50. ↑ Baragiola, R. A.; Duke, C. A.; Loeffler, M.; McFadden, L. A.; Sheffield, J. (2003). "Impact of ions and micrometeorites on mineral surfaces: Reflectance changes and production of atmospheric species in airless solar system bodies". EGS – AGU – EUG Joint Assembly: 7709. Bibcode: 2003EAEJA.....7709B. 
  51. ↑ Chapman, C. R.; Williams, J. G.; Hartmann, W. K. (1978). "The asteroids". Annual Review of Astronomy and Astrophysics 16: 33–75. doi:10.1146/annurev.aa.16.090178.000341. Bibcode: 1978ARA&A..16...33C. 
  52. ↑ Kracher, A. (2005). "Asteroid 433 Eros and partially differentiated planetesimals: bulk depletion versus surface depletion of sulfur". Ames Laboratory. http://www.cosis.net/abstracts/EGU05/03788/EGU05-J-03788.pdf. 
  53. ↑ Piccioni, Robert (2012-11-19). "Did Asteroid Impacts Make Earth Habitable?". Guidetothecosmos.com. http://www.guidetothecosmos.com/newsletter-Habitable-Earth.html. 
  54. ↑ Stiles, Lori (September 15, 2005). "Asteroids Caused the Early Inner Solar System Cataclysm" (in en). UANews. https://uanews.arizona.edu/story/asteroids-caused-early-inner-solar-system-cataclysm. 
  55. ↑ Alfvén, H.; Arrhenius, G. (1976). "The Small Bodies". SP-345 Evolution of the Solar System. NASA. https://history.nasa.gov/SP-345/ch4.htm. 
  56. ↑ 56.0 56.1 Spratt, Christopher E. (April 1990). "The Hungaria group of minor planets". Journal of the Royal Astronomical Society of Canada 84: 123–131. Bibcode: 1990JRASC..84..123S. 
  57. ↑ Lecar, M.; Podolak, M.; Sasselov, D.; Chiang, E. (2006). "Infrared cirrus – New components of the extended infrared emission". The Astrophysical Journal 640 (2): 1115–1118. doi:10.1086/500287. Bibcode: 2006ApJ...640.1115L. 
  58. ↑ Berardelli, Phil (March 23, 2006). "Main-Belt Comets May Have Been Source Of Earths Water". Space Daily. http://www.spacedaily.com/reports/Main_Belt_Comets_May_Have_Been_Source_Of_Earths_Water.html. 
  59. ↑ Lakdawalla, Emily (April 28, 2006). "Discovery of a Whole New Type of Comet". The Planetary Society. http://www.planetary.org/blog/article/00000551/. 
  60. ↑ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 October 2022). "Recent arrivals to the main asteroid belt". Celestial Mechanics and Dynamical Astronomy 134 (5): 38. doi:10.1007/s10569-022-10094-4. Bibcode: 2022CeMDA.134...38D. 
  61. ↑ Davis, D. R.; Durda, D. D.; Marzari, F.; Campo Bagatin, A.; Gil-Hutton, R. (March 2002). "Collisional Evolution of Small-Body Populations". in Bottke Jr., W. F.; Cellino, A.; Paolicchi, P. et al.. Asteroids III. Tucson: University of Arizona Press. pp. 545–558. doi:10.2307/j.ctv1v7zdn4.41. Bibcode: 2002aste.book..545D. https://www.lpi.usra.edu/books/AsteroidsIII/pdf/3029.pdf. Retrieved 2023-02-11. 
  62. ↑ Yeomans, Donald K. (April 26, 2007). "JPL Small-Body Database Search Engine". NASA JPL. http://ssd.jpl.nasa.gov/sbdb_query.cgi.  – search for asteroids in the main belt regions with a diameter >100.
  63. ↑ Tedesco, E. F.; Desert, F.-X. (2002). "The Infrared Space Observatory Deep Asteroid Search". The Astronomical Journal 123 (4): 2070–2082. doi:10.1086/339482. Bibcode: 2002AJ....123.2070T. 
  64. ↑ Bottkejr, W.; Durda, D.; Nesvorny, D.; Jedicke, R.; Morbidelli, A.; Vokrouhlicky, D.; Levison, H. (May 2005). "The fossilized size distribution of the main asteroid belt" (in en). Icarus 175 (1): 111–140. doi:10.1016/j.icarus.2004.10.026. Bibcode: 2005Icar..175..111B. https://linkinghub.elsevier.com/retrieve/pii/S0019103504003811. 
  65. ↑ O'Brien, David P.; Sykes, Mark V. (December 2011). "The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres" (in en). Space Science Reviews 163 (1–4): 41–61. doi:10.1007/s11214-011-9808-6. ISSN 0038-6308. Bibcode: 2011SSRv..163...41O. http://link.springer.com/10.1007/s11214-011-9808-6. 
  66. ↑ 66.0 66.1 Williams, Gareth (September 25, 2010). "Distribution of the Minor Planets". Minor Planets Center. http://www.minorplanetcenter.org/iau/lists/MPDistribution.html. 
  67. ↑ "The asteroid belt contains solar system remnants". 2021-11-03. https://earthsky.org/space/what-is-the-asteroid-belt/. 
  68. ↑ Williams, Matt (2016-08-10). "How Far is the Asteroid Belt from Earth?". https://www.universetoday.com/130136/far-asteroid-belt-earth/. 
  69. ↑ "In Depth | Ceres". https://solarsystem.nasa.gov/planets/dwarf-planets/ceres/in-depth. 
  70. ↑ Gradie, J.; Tedesco, E. (June 1982). "Compositional Structure of the Asteroid Belt". Science 216 (4553): 1405–1407. doi:10.1126/science.216.4553.1405. PMID 17798362. Bibcode: 1982Sci...216.1405G. 
  71. ↑ 71.0 71.1 71.2 DeMeo, F. E.; Alexander, C. M. O'D.; Walsh, K. J.; Chapman, C. R.; Binzel, R. P. (2015). "The Compositional Structure of the Asteroid Belt". in Michel, Patrick; DeMeo, Francesca E.; Bottke, William F.. Asteroids IV. Tucson: University of Arizona Press. pp. 13–41. doi:10.2458/azu_uapress_9780816532131-ch002. ISBN 978-0-816-53213-1. Bibcode: 2015aste.book...13D. 
  72. ↑ 72.0 72.1 Wiegert, P.; Balam, D.; Moss, A.; Veillet, C.; Connors, M.; Shelton, I. (2007). "Evidence for a Color Dependence in the Size Distribution of Main-Belt Asteroids". The Astronomical Journal 133 (4): 1609–1614. doi:10.1086/512128. Bibcode: 2007AJ....133.1609W. http://astro.uwo.ca/~wiegert/papers/2007AJ.133.1609.pdf. Retrieved 2008-09-06. 
  73. ↑ 73.0 73.1 73.2 Blair, Edward C., ed (2002). Asteroids: Overview, Abstracts, and Bibliography. Nova Science Publishers. p. 2. ISBN 978-1-59033-482-9. https://books.google.com/books?id=oa289IxCvAAC&pg=PA2. 
  74. ↑ Clark, B. E. (1996). "New News and the Competing Views of Asteroid Belt Geology". Lunar and Planetary Science 27: 225–226. Bibcode: 1996LPI....27..225C. 
  75. ↑ Margot, J. L.; Brown, M. E. (2003). "A Low-Density M-type Asteroid in the Main Belt". Science 300 (5627): 1939–1942. doi:10.1126/science.1085844. PMID 12817147. Bibcode: 2003Sci...300.1939M. https://pdfs.semanticscholar.org/d014/0c3feee1d41f01ff67e1637b4d367da520ef.pdf. 
  76. ↑ 76.0 76.1 Lang, Kenneth R. (2003). "Asteroids and meteorites". NASA's Cosmos. http://ase.tufts.edu/cosmos/print_images.asp?id=15. 
  77. ↑ Mueller, M.; Harris, A. W.; Delbo, M. (2005). the MIRSI Team. "21 Lutetia and other M-types: Their sizes, albedos, and thermal properties from new IRTF measurements". Bulletin of the American Astronomical Society 37: 627. Bibcode: 2005DPS....37.0702M. 
  78. ↑ 78.0 78.1 Duffard, R. D.; Roig, F. (July 14–18, 2008). "Two New Basaltic Asteroids in the Main Belt?". Baltimore, Maryland. Bibcode: 2008LPICo1405.8154D. 
  79. ↑ 79.0 79.1 Than, Ker (2007). "Strange Asteroids Baffle Scientists". space.com. http://www.space.com/scienceastronomy/070821_basalt_asteroid.html. 
  80. ↑ "When is a comet not a comet?". ESA/Hubble Press Release. http://www.spacetelescope.org/news/heic1320/. 
  81. ↑ Low, F. J.; Beintema, D. A.; Gautier, T. N.; Gillett, F. C.; Beichman, C. A.; Neugebauer, G.; Young, E.; Aumann, H. H. (1984). "Infrared cirrus – New components of the extended infrared emission". Astrophysical Journal Letters 278: L19–L22. doi:10.1086/184213. Bibcode: 1984ApJ...278L..19L. 
  82. ↑ "Interview with David Jewitt". YouTube.com. 2007-01-05. https://www.youtube.com/watch?v=B1W4NTmI5Bk. 
  83. ↑ This value was obtained by a simple count of all bodies in that region using data for 120,437 numbered minor planets from the Minor Planet Center orbit database, dated February 8, 2006.
  84. ↑ "JPL Small-Body Database Search Engine: orbital class (MBA)". JPL Solar System Dynamics. http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=all;obj_numbered=all;ast_orbit_class=MBA;OBJ_field=0;ORB_field=0;table_format=HTML;max_rows=100;format_option=comp;c_fields=AcBhBgBjBiBnBsCkCqAi;.cgifields=format_option;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=com_orbit_class&query=1&c_sort=AcA. 
  85. ↑ Fernie, J. Donald (1999). "The American Kepler". American Scientist 87 (5): 398. doi:10.1511/1999.5.398. http://www.americanscientist.org/issues/pub/1999/9/the-american-kepler/2. Retrieved 2007-02-04. 
  86. ↑ Liou, Jer-Chyi; Malhotra, Renu (1997). "Depletion of the Outer Asteroid Belt". Science 275 (5298): 375–377. doi:10.1126/science.275.5298.375. PMID 8994031. Bibcode: 1997Sci...275..375L. 
  87. ↑ Backman, D. E. (March 6, 1998). "Fluctuations in the General Zodiacal Cloud Density". Backman Report. NASA Ames Research Center. http://astrobiology.arc.nasa.gov/workshops/zodiac/backman/backman_toc.html. 
  88. ↑ Nesvorný, David; Bottke Jr, William F.; Dones, Luke; Levison, Harold F. (June 2002). "The recent breakup of an asteroid in the main-belt region". Nature 417 (6890): 720–722. doi:10.1038/nature00789. PMID 12066178. Bibcode: 2002Natur.417..720N. http://www.boulder.swri.edu/~davidn/papers/nesvorny-etal-karin-nature-2002.pdf. 
  89. ↑ Walsh, Kevin J. (September 2018). "Rubble Pile Asteroids". Annual Review of Astronomy and Astrophysics 56: 593–624. doi:10.1146/annurev-astro-081817-052013. Bibcode: 2018ARA&A..56..593W. 
  90. ↑ 90.0 90.1 Reach, William T. (1992). "Zodiacal emission. III – Dust near the asteroid belt". Astrophysical Journal 392 (1): 289–299. doi:10.1086/171428. Bibcode: 1992ApJ...392..289R. 
  91. ↑ Nesvorný, David; Jenniskens, Peter; Levison, Harold F.; Bottke, William F.; Vokrouhlický, David; Gounelle, Matthieu (2010). "Cometary Origin of the Zodiacal Cloud and Carbonaceous Micrometeorites. Implications for Hot Debris Disks". The Astrophysical Journal 713 (2): 816–836. doi:10.1088/0004-637X/713/2/816. Bibcode: 2010ApJ...713..816N. 
  92. ↑ Kingsley, Danny (May 1, 2003). "Mysterious meteorite dust mismatch solved". ABC Science. http://abc.net.au/science/news/stories/s843594.htm. 
  93. ↑ "Meteors and Meteorites". NASA. http://www.nasa.gov/pdf/145945main_Meteors.Meteorites.Lithograph.pdf. 
  94. ↑ Hughes, David W. (2007). "Finding Asteroids In Space". BBC. http://www.open2.net/sciencetechnologynature/planetsbeyond/asteroids/finding.html. 
  95. ↑ Lemaitre, Anne (August 31 – September 4, 2004). "Asteroid family classification from very large catalogues". Belgrade, Serbia and Montenegro: Cambridge University Press. pp. 135–144. doi:10.1017/S1743921304008592. Bibcode: 2005dpps.conf..135L. 
  96. ↑ Martel, Linda M. V. (March 9, 2004). "Tiny Traces of a Big Asteroid Breakup". Planetary Science Research Discoveries. http://www.psrd.hawaii.edu/Mar04/fossilMeteorites.html. 
  97. ↑ Drake, Michael J. (2001). "The eucrite/Vesta story". Meteoritics & Planetary Science 36 (4): 501–513. doi:10.1111/j.1945-5100.2001.tb01892.x. Bibcode: 2001M&PS...36..501D. 
  98. ↑ Love, S. G.; Brownlee, D. E. (1992). "The IRAS dust band contribution to the interplanetary dust complex – Evidence seen at 60 and 100 microns". Astronomical Journal 104 (6): 2236–2242. doi:10.1086/116399. Bibcode: 1992AJ....104.2236L. 
  99. ↑ Galiazzo, M. A.; Wiegert, P.; Aljbaae, S. (2016). "Influence of the Centaurs and TNOs on the main belt and its families". Astrophysics and Space Science 361 (12): 361–371. doi:10.1007/s10509-016-2957-z. Bibcode: 2016Ap&SS.361..371G. 
  100. ↑ Carvano, J. M.; Lazzaro, D.; Mothé-Diniz, T.; Angeli, C. A.; Florczak, M. (2001). "Spectroscopic Survey of the Hungaria and Phocaea Dynamical Groups". Icarus 149 (1): 173–189. doi:10.1006/icar.2000.6512. Bibcode: 2001Icar..149..173C. 
  101. ↑ Bojan Novaković, Georgios Tsirvoulis, Mikael Granvik, and Ana Todović (2017-05-25). "A Dark Asteroid Family in the Phocaea Region". The Astronomical Journal 153 (6): 266. doi:10.3847/1538-3881/aa6ea8. Bibcode: 2017AJ....153..266N. 
  102. ↑ Dymock, Roger (2010). Asteroids and Dwarf Planets and How to Observe Them. Astronomers' Observing Guides. Springer. p. 24. ISBN 978-1-4419-6438-0. https://books.google.com/books?id=vQcAnwt_87sC&pg=PA24. Retrieved 2011-04-04. 
  103. ↑ Nesvorný, David; Enke, Brian L.; Bottke, William F.; Durda, Daniel D.; Asphaug, Erik; Richardson, Derek C. (August 2006). "Karin cluster formation by asteroid impact". Icarus 183 (2): 296–311. doi:10.1016/j.icarus.2006.03.008. Bibcode: 2006Icar..183..296N. 
  104. ↑ McKee, Maggie (January 18, 2006). "Eon of dust storms traced to asteroid smash". New Scientist Space. https://www.newscientist.com/channel/solar-system/comets-asteroids/dn8603. 
  105. ↑ Nesvorný, D.; Vokrouhlický, D.; Bottke, W. F. (2006). "The Breakup of a Main-Belt Asteroid 450 Thousand Years Ago". Science 312 (5779): 1490. doi:10.1126/science.1126175. PMID 16763141. Bibcode: 2006Sci...312.1490N. http://www.boulder.swri.edu/~bottke/Reprints/Nesvorny_Vok_Bottke_Science_2006_Datura_breakup.pdf. 
  106. ↑ Vokrouhlický, D.; Durech, J.; Michałowski, T.; Krugly, Yu. N.; Gaftonyuk, N. M.; Kryszczyńska, A.; Colas, F.; Lecacheux, J. et al. (2009). "Datura family: the 2009 update". Astronomy & Astrophysics 507 (1): 495–504. doi:10.1051/0004-6361/200912696. Bibcode: 2009A&A...507..495V. https://www.aanda.org/articles/aa/full_html/2009/43/aa12696-09/aa12696-09.html. 
  107. ↑ Nesvorný, D.; Bottke, W. F.; Levison, H. F.; Dones, L. (2003). "Recent Origin of the Solar System Dust Bands". The Astrophysical Journal 591 (1): 486–497. doi:10.1086/374807. Bibcode: 2003ApJ...591..486N. http://pdfs.semanticscholar.org/7bb5/43a73044fcef4e52ab6b95c378ca617c93f7.pdf. 
  108. ↑ Schippers, P.; Meyer-Vernet, N.; Lecacheux, A.; Belheouane, S.; Moncuquet, M.; Kurth, W. S.; Mann, I.; Mitchell, D. G. et al. (June 2015). "Nanodust Detection between 1 and 5 AU Using Cassini Wave Measurements". The Astrophysical Journal 806 (1): 77. doi:10.1088/0004-637X/806/1/77. 77. Bibcode: 2015ApJ...806...77S. 
  109. ↑ Greicius, Tony (July 31, 2015). "NASA's Juno Gives Starship-Like View of Earth Flyby". NASA. http://www.nasa.gov/jpl/juno/juno-earth-flyby-20131210.html. 
  110. ↑ Stern, Alan (June 2, 2006). "New Horizons Crosses The Asteroid Belt". Space Daily. http://www.spacedaily.com/reports/New_Horizons_Crosses_The_Asteroid_Belt.html. 
  111. ↑ Barucci, M. A.; Fulchignoni, M.; Rossi, A. (2007). "Rosetta Asteroid Targets: 2867 Steins and 21 Lutetia". Space Science Reviews 128 (1–4): 67–78. doi:10.1007/s11214-006-9029-6. Bibcode: 2007SSRv..128...67B. 
  112. ↑ "NASA's Lucy Team Announces New Asteroid Target". NASA. January 25, 2023. https://www.nasa.gov/feature/goddard/2023/nasa-s-lucy-team-announces-new-asteroid-target. 
  113. ↑ Avdellidou, C.; Pajola, M.; Lucchetti, A.; Agostini, L.; Delbo, M.; Mazzotta Epifani, E.; Bourdelle De Micas, J.; Devogèle, M. et al. (2021). "Characterisation of the main belt asteroid (223) Rosa". Astronomy & Astrophysics 656: L18. doi:10.1051/0004-6361/202142600. Bibcode: 2021A&A...656L..18A. 
  114. ↑ "NASA Continues Psyche Asteroid Mission". NASA. October 28, 2022. https://www.jpl.nasa.gov/news/nasa-continues-psyche-asteroid-mission. 

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