What are Asteroid?
Animation of asteroid 433 Eros in rotation.
Asteroids are
minor planets (
small Solar System bodies and
dwarf planets) that are not
comets, especially those of the
inner Solar System. They have also been called
planetoids, especially the larger ones. These terms have historically been applied to any astronomical object orbiting the
Sun
that did not show the disk of a planet and was not observed to have the
characteristics of an active comet, but as small objects in the
outer Solar System were discovered, their
volatile-based surfaces were found to more closely resemble comets, and so were often distinguished from traditional asteroids.
[1] Thus the term
asteroid has come increasingly to refer specifically to the small bodies of the inner Solar System out to the orbit of
Jupiter. They are grouped with the outer bodies—
centaurs,
Neptune trojans, and
trans-Neptunian objects—as minor planets, which is the term preferred in astronomical circles.
[2] In this article the term "asteroid" refers to the minor planets of the inner Solar System.
There are millions of asteroids, many thought to be the shattered remnants of
planetesimals, bodies within the young Sun's
solar nebula that never grew large enough to become
planets.
[3] The large majority of known asteroids orbit in the
asteroid belt between the orbits of Mars and Jupiter or co-orbital with Jupiter (the
Jupiter Trojans). However, other orbital families exist with significant populations, including the
near-Earth asteroids. Individual asteroids are classified by their characteristic
spectra, with the majority falling into three main groups:
C-type,
S-type, and
M-type. These were named after and are generally identified with
carbon-rich,
stony, and
metallic compositions, respectively.
Only one asteroid,
4 Vesta,
which has a relatively reflective surface, is normally visible to the
naked eye, and this only in very dark skies when it is favorably
positioned. Rarely, small asteroids passing close to Earth may be
naked-eye visible for a short time.
[4]
Naming
2013 EC, shown here in radar images, has a provisional designation
A newly discovered asteroid is given a
provisional designation (such as
2002 AT4)
consisting of the year of discovery and an alphanumeric code indicating
the half-month of discovery and the sequence within that half-month.
Once an asteroid's orbit has been confirmed, it is given a number, and
later may also be given a name (e.g.
433 Eros).
The formal naming convention uses parentheses around the number (e.g.
(433) Eros), but dropping the parentheses is quite common. Informally,
it is common to drop the number altogether, or to drop it after the
first mention when a name is repeated in running text.
Symbols
The first asteroids to be discovered were assigned iconic symbols
like the ones traditionally used to designate the planets. By 1855 there
were two dozen asteroid symbols, which often occurred in multiple
variants.
[5]
| Asteroid |
Symbol |
Year |
| Ceres |
⚳    |
Ceres' scythe, reversed to double as the letter C |
1801 |
| 2 Pallas |
⚴   |
Athena's (Pallas') spear |
1801 |
| 3 Juno |
⚵    |
A star mounted on a scepter,
for Juno, the Queen of Heaven |
1804 |
| 4 Vesta |
⚶     |
The altar and sacred fire of Vesta |
1807 |
| 5 Astraea |
  |
A scale, or an inverted anchor, symbols of justice |
1845 |
| 6 Hebe |
 |
Hebe's cup |
1847 |
| 7 Iris |
 |
A rainbow (iris) and a star |
1847 |
| 8 Flora |
 |
A flower (flora) (specifically the Rose of England) |
1847 |
| 9 Metis |
 |
The eye of wisdom and a star |
1848 |
| 10 Hygiea |
  |
Hygiea's serpent and a star, or the Rod of Asclepius |
1849 |
| 11 Parthenope |
  |
A harp, or a fish and a star; symbols of the sirens |
1850 |
| 12 Victoria |
 |
The laurels of victory and a star |
1850 |
| 13 Egeria |
 |
A shield, symbol of Egeria's protection, and a star |
1850 |
| 14 Irene |
 |
A dove carrying an olive branch (symbol of
irene 'peace') with a star on its head,[6] or
an olive branch, a flag of truce, and a star |
1851 |
| 15 Eunomia |
 |
A heart, symbol of good order
(eunomia), and a star |
1851 |
| 16 Psyche |
 |
A butterfly's wing, symbol of
the soul (psyche), and a star |
1852 |
| 17 Thetis |
 |
A dolphin, symbol of Thetis, and a star |
1852 |
| 18 Melpomene |
 |
The dagger of Melpomene, and a star |
1852 |
| 19 Fortuna |
 |
The wheel of fortune and a star |
1852 |
| 26 Proserpina |
 |
Proserpina's pomegranate |
1853 |
| 28 Bellona |
 |
Bellona's whip and lance[7] |
1854 |
| 29 Amphitrite |
 |
The shell of Amphitrite and a star |
1854 |
| 35 Leukothea |
 |
A lighthouse beacon, symbol of Leucothea[8] |
1855 |
| 37 Fides |
 |
The cross of faith (fides)[9] |
1855 |
In 1851,
[10] after the fifteenth asteroid (
Eunomia) had been discovered,
Johann Franz Encke made a major change in the upcoming 1854 edition of the
Berliner Astronomisches Jahrbuch (BAJ,
Berlin Astronomical Yearbook).
He introduced a disk (circle), a traditional symbol for a star, as the
generic symbol for an asteroid. The circle was then numbered in order of
discovery to indicate a specific asteroid (although he assigned ① to
the fifth,
Astraea,
while continuing to designate the first four only with their existing
iconic symbols). The numbered-circle convention was quickly adopted by
astronomers, and the next asteroid to be discovered (
16 Psyche,
in 1852) was the first to be designated in that way at the time of its
discovery. However, Psyche was also given an iconic symbol, as were a
few other asteroids discovered over the next few years (see chart
above).
20 Massalia
was the first asteroid that was not assigned a symbol, and no
additional iconic symbols were created after the 1855 discovery of
37 Fides.
[11]
That year Astraea's number was increased to ⑤, but the first four
asteroid, Ceres to Vesta, were not listed by their numbers until the
1867 edition. The circle became a pair of parentheses, and the
parentheses were sometimes omitted altogether over the next few decades,
leading to the modern convention.
[6]
Discovery
243 Ida and its moon Dactyl. Dactyl is the first satellite of an asteroid to be discovered.
The first asteroid to be discovered,
Ceres, was found in 1801 by
Giuseppe Piazzi, and was originally considered to be a new planet.
[note 1]
This was followed by the discovery of other similar bodies, which, with
the equipment of the time, appeared to be points of light, like stars,
showing little or no planetary disc, though readily distinguishable from
stars due to their apparent motions. This prompted the astronomer
Sir William Herschel to propose the term "asteroid", coined in Greek as ἀστεροειδής
asteroeidēs 'star-like, star-shaped', from Ancient Greek
ἀστήρ astēr
'star, planet'. In the early second half of the nineteenth century, the
terms "asteroid" and "planet" (not always qualified as "minor") were
still used interchangeably; for example, the
Annual of Scientific Discovery for 1871,
page 316, reads "Professor J. Watson has been awarded by the Paris
Academy of Sciences, the astronomical prize, Lalande foundation, for the
discovery of eight new asteroids in one year. The planet Lydia (No.
110), discovered by M. Borelly at the Marseilles Observatory [...] M.
Borelly had previously discovered two planets bearing the numbers 91 and
99 in the system of asteroids revolving between Mars and Jupiter".
Historical methods
Asteroid discovery methods have dramatically improved over the past two centuries.
In the last years of the 18th century, Baron
Franz Xaver von Zach organized a group of 24 astronomers to search the sky for the missing planet predicted at about 2.8
AU from the Sun by the
Titius-Bode law, partly because of the discovery, by Sir
William Herschel in 1781, of the planet
Uranus at the distance predicted by the law. This task required that hand-drawn sky charts be prepared for all stars in the
zodiacal
band down to an agreed-upon limit of faintness. On subsequent nights,
the sky would be charted again and any moving object would, hopefully,
be spotted. The expected motion of the missing planet was about 30
seconds of arc per hour, readily discernible by observers.
The first object,
Ceres, was not discovered by a member of the group, but rather by accident in 1801 by
Giuseppe Piazzi, director of the observatory of
Palermo in
Sicily. He discovered a new star-like object in
Taurus and followed the displacement of this object during several nights. His colleague,
Carl Friedrich Gauss,
used these observations to find the exact distance from this unknown
object to the Earth. Gauss' calculations placed the object between the
planets
Mars and
Jupiter. Piazzi named it after
Ceres, the Roman goddess of agriculture.
Three other asteroids (
2 Pallas,
3 Juno, and
4 Vesta)
were discovered over the next few years, with Vesta found in 1807.
After eight more years of fruitless searches, most astronomers assumed
that there were no more and abandoned any further searches.
However,
Karl Ludwig Hencke persisted, and began searching for more asteroids in 1830. Fifteen years later, he found
5 Astraea, the first new asteroid in 38 years. He also found
6 Hebe
less than two years later. After this, other astronomers joined in the
search and at least one new asteroid was discovered every year after
that (except the wartime year 1945). Notable asteroid hunters of this
early era were
J. R. Hind,
Annibale de Gasparis,
Robert Luther,
H. M. S. Goldschmidt,
Jean Chacornac,
James Ferguson,
Norman Robert Pogson,
E. W. Tempel,
J. C. Watson,
C. H. F. Peters,
A. Borrelly,
J. Palisa, the
Henry brothers and
Auguste Charlois.
In 1891, however,
Max Wolf pioneered the use of
astrophotography
to detect asteroids, which appeared as short streaks on long-exposure
photographic plates. This dramatically increased the rate of detection
compared with earlier visual methods: Wolf alone discovered 248
asteroids, beginning with
323 Brucia,
whereas only slightly more than 300 had been discovered up to that
point. It was known that there were many more, but most astronomers did
not bother with them
[citation needed], calling them "vermin of the skies", a phrase variously attributed to
Eduard Suess[12] and
Edmund Weiss.
[13] Even a century later, only a few thousand asteroids were identified, numbered and named.
Manual methods of the 1900s and modern reporting
Until 1998, asteroids were discovered by a four-step process. First, a region of the sky was
photographed by a wide-field
telescope, or
Astrograph.
Pairs of photographs were taken, typically one hour apart. Multiple
pairs could be taken over a series of days. Second, the two films or
plates of the same region were viewed under a
stereoscope.
Any body in orbit around the Sun would move slightly between the pair
of films. Under the stereoscope, the image of the body would seem to
float slightly above the background of stars. Third, once a moving body
was identified, its location would be measured precisely using a
digitizing microscope. The location would be measured relative to known
star locations.
[14]
These first three steps do not constitute asteroid discovery: the observer has only found an apparition, which gets a
provisional designation,
made up of the year of discovery, a letter representing the half-month
of discovery, and finally a letter and a number indicating the
discovery's sequential number (example:
1998 FJ74).
The last step of discovery is to send the locations and time of observations to the
Minor Planet Center,
where computer programs determine whether an apparition ties together
earlier apparitions into a single orbit. If so, the object receives a
catalogue number and the observer of the first apparition with a
calculated orbit is declared the discoverer, and granted the honor of
naming the object subject to the approval of the
International Astronomical Union.
Computerized methods
There is increasing interest in identifying asteroids whose orbits cross
Earth's, and that could, given enough time, collide with Earth (see
Earth-crosser asteroids). The three most important groups of
near-Earth asteroids are the
Apollos,
Amors, and
Atens. Various
asteroid deflection strategies have been proposed, as early as the 1960s.
The
near-Earth asteroid
433 Eros had been discovered as long ago as 1898, and the 1930s brought a flurry of similar objects. In order of discovery, these were:
1221 Amor,
1862 Apollo,
2101 Adonis, and finally
69230 Hermes, which approached within 0.005
AU of the
Earth in 1937. Astronomers began to realize the possibilities of Earth impact.
Two events in later decades increased the alarm: the increasing acceptance of
Walter Alvarez' hypothesis that an
impact event resulted in the
Cretaceous–Paleogene extinction, and the 1994 observation of
Comet Shoemaker-Levy 9 crashing into
Jupiter.
The U.S. military also declassified the information that its military
satellites, built to detect nuclear explosions, had detected hundreds of
upper-atmosphere impacts by objects ranging from one to 10 metres
across.
All these considerations helped spur the launch of highly efficient automated systems that consist of Charge-Coupled Device (
CCD)
cameras and computers directly connected to telescopes. Since 1998, a
large majority of the asteroids have been discovered by such automated
systems. A list of teams using such automated systems includes:
[15]
The LINEAR system alone has discovered 121,346 asteroids, as of March, 2011.
[16] Among all the automated systems, 4711 near-Earth asteroids have been discovered
[17] including over 600 more than 1 km (0.6 mi) in diameter.
Terminology
A composite image, to
scale, of the asteroids which have been imaged at high resolution. As of
2011 they are, from largest to smallest:
4 Vesta,
21 Lutetia,
253 Mathilde,
243 Ida and its moon Dactyl,
433 Eros,
951 Gaspra,
2867 Šteins,
25143 Itokawa.
The largest asteroid in the previous image,
Vesta (left), with
Ceres (center) and Earth's
Moon (right) shown to scale.
Traditionally, small bodies orbiting the Sun were classified as asteroids,
comets or
meteoroids, with anything smaller than ten metres across being called a meteoroid.
[18] The term "asteroid" is ill-defined. It never had a formal definition, with the broader term
minor planet being preferred by the
International Astronomical Union from 1853 on. In 2006, the term "
small Solar System body" was introduced to cover both most minor planets and comets.
[19]
Other languages prefer "planetoid" (Greek for "planet-like"), and this
term is occasionally used in English for larger minor planets such as
the
dwarf planets. The word "
planetesimal"
has a similar meaning, but refers specifically to the small building
blocks of the planets that existed when the Solar System was forming.
The term "planetule" was coined by the geologist
William Daniel Conybeare to describe minor planets,
[20] but is not in common use. The three largest objects in the asteroid belt,
Ceres,
2 Pallas, and
4 Vesta, grew to the stage of
protoplanets. Ceres has been classified as a
dwarf planet, the only one in the inner Solar System.
When found, asteroids were seen as a class of objects distinct from
comets, and there was no unified term for the two until "small Solar
System body" was coined in 2006. The main difference between an asteroid
and a comet is that a comet shows a coma due to
sublimation
of near surface ices by solar radiation. A few objects have ended up
being dual-listed because they were first classified as minor planets
but later showed evidence of cometary activity. Conversely, some
(perhaps all) comets are eventually depleted of their surface
volatile ices
and become asteroids. A further distinction is that comets typically
have more eccentric orbits than most asteroids; most "asteroids" with
notably eccentric orbits are probably dormant or extinct comets.
[21]
For almost two centuries, from the discovery of
Ceres in 1801 until the discovery of the first
centaur,
2060 Chiron, in 1977, all known asteroids spent most of their time at or within the orbit of Jupiter, though a few such as
944 Hidalgo
ventured far beyond Jupiter for part of their orbit. When astronomers
started finding more small bodies that permanently resided further out
than Jupiter, now called
centaurs,
they numbered them among the traditional asteroids, though there was
debate over whether they should be classified as asteroids or as a new
type of object. Then, when the first
trans-Neptunian object,
1992 QB1,
was discovered in 1992, and especially when large numbers of similar
objects started turning up, new terms were invented to sidestep the
issue:
Kuiper-belt object,
trans-Neptunian object,
scattered-disc object,
and so on. These inhabit the cold outer reaches of the Solar System
where ices remain solid and comet-like bodies are not expected to
exhibit much cometary activity; if centaurs or trans-Neptunian objects
were to venture close to the Sun, their volatile ices would sublimate,
and traditional approaches would classify them as comets and not
asteroids.
The innermost of these are the
Kuiper-belt objects, called "objects" partly to avoid the need to classify them as asteroids or comets.
[22] They are believed to be predominantly comet-like in composition, though some may be more akin to asteroids.
[23]
Furthermore, most do not have the highly eccentric orbits associated
with comets, and the ones so far discovered are larger than traditional
comet nuclei. (The much more distant
Oort cloud
is hypothesized to be the main reservoir of dormant comets.) Other
recent observations, such as the analysis of the cometary dust collected
by the
Stardust probe, are increasingly blurring the distinction between comets and asteroids,
[24] suggesting "a continuum between asteroids and comets" rather than a sharp dividing line.
[25]
The minor planets beyond Jupiter's orbit are sometimes also called "asteroids", especially in popular presentations.
[26]
However, it is becoming increasingly common for the term "asteroid" to
be restricted to minor planets of the inner Solar System.
[22] Therefore, this article will restrict itself for the most part to the classical asteroids: objects of the
asteroid belt,
Jupiter trojans, and
near-Earth objects.
When the IAU introduced the class
small Solar System bodies in 2006 to include most objects previously classified as minor planets and comets, they created the class of
dwarf planets
for the largest minor planets—those that have enough mass to have
become ellipsoidal under their own gravity. According to the IAU, "the
term 'minor planet' may still be used, but generally the term 'Small
Solar System Body' will be preferred."
[27] Currently only the largest object in the asteroid belt,
Ceres, at about 950 km (590 mi) across, has been placed in the dwarf planet category, although there are several large asteroids (
Vesta,
Pallas, and
Hygiea) that may be classified as dwarf planets when their shapes are better known.
[28]
Formation
It is believed that
planetesimals in the asteroid belt evolved much like the rest of the
solar nebula until Jupiter neared its current mass, at which point excitation from
orbital resonances
with Jupiter ejected over 99% of planetesimals in the belt. Simulations
and a discontinuity in spin rate and spectral properties suggest that
asteroids larger than approximately 120 km (75 mi) in diameter accreted
during that early era, whereas smaller bodies are fragments from
collisions between asteroids during or after the Jovian disruption.
[29] Ceres and Vesta grew large enough to melt and
differentiate, with heavy metallic elements sinking to the core, leaving rocky minerals in the crust.
[30]
In the
Nice model, many
Kuiper-belt objects
are captured in the outer asteroid belt, at distances greater than 2.6
AU. Most were later ejected by Jupiter, but those that remained may be
the
D-type asteroids, and possibly include Ceres.
[31]
Distribution within the Solar System
Various dynamical groups of asteroids have been discovered orbiting
in the inner Solar System. Their orbits are perturbed by the gravity of
other bodies in the Solar System and by the
Yarkovsky effect. Significant populations include:
Asteroid belt
Main article:
Asteroid belt
The majority of known asteroids orbit within the asteroid belt between the orbits of
Mars and
Jupiter, generally in relatively low-
eccentricity
(i.e. not very elongated) orbits. This belt is now estimated to contain
between 1.1 and 1.9 million asteroids larger than 1 km (0.6 mi) in
diameter,
[32] and millions of smaller ones. These asteroids may be remnants of the
protoplanetary disk, and in this region the
accretion of
planetesimals into planets during the formative period of the Solar System was prevented by large gravitational perturbations by
Jupiter.
Trojans
Trojan asteroids are a population that share an orbit with a larger
planet or moon, but do not collide with it because they orbit in one of
the two
Lagrangian points of stability,
L4 and L5, which lie 60° ahead of and behind the larger body.
The most significant population of Trojan asteroids are the
Jupiter Trojans.
Although fewer Jupiter Trojans have been discovered as of 2010, it is
thought that they are as numerous as the asteroids in the asteroid belt.
A couple of
trojans have also been found orbiting with
Mars.
[note 2]
Near-Earth asteroids
Near-Earth asteroids, or NEAs, are asteroids that have orbits that
pass close to that of Earth. Asteroids that actually cross the Earth's
orbital path are known as
Earth-crossers. As of May 2010, 7,075
near-Earth asteroids are known and the number over one kilometre in
diameter is estimated to be 500–1,000.
Characteristics
Size distribution
Sizes of the first ten asteroids to be discovered, compared to the Earth's Moon
HST image of the dwarf planet Ceres
Asteroids vary greatly in size, from almost 1000 kilometres for the largest down to rocks just tens of metres across.
[note 3]
The three largest are very much like miniature planets: they are
roughly spherical, have at least partly differentiated interiors,
[33] and are thought to be surviving
protoplanets. The vast majority, however, are much smaller and are irregularly shaped; they are thought to be either surviving
planetesimals or fragments of larger bodies.
The
dwarf planet Ceres is by far the largest asteroid, with a diameter of 975 km (610 mi). The next largest are
2 Pallas and
4 Vesta,
both with diameters of just over 500 km (300 mi). Vesta is the only
main-belt asteroid that can, on occasion, be visible to the naked eye.
On some rare occasions, a near-Earth asteroid may briefly become visible
without technical aid; see
99942 Apophis.
The mass of all the objects of the
asteroid belt, lying between the orbits of
Mars and
Jupiter, is estimated to be about 2.8–3.2
×10
21 kg, or about 4 percent of the mass of the Moon. Of this,
Ceres comprises 0.95
×10
21 kg, a third of the total.
[34] Adding in the next three most massive objects,
Vesta (9%),
Pallas (7%), and
Hygiea (3%), brings this figure up to 51%; while the three after that,
511 Davida (1.2%),
704 Interamnia (1.0%), and
52 Europa
(0.9%), only add another 3% to the total mass. The number of asteroids
then increases rapidly as their individual masses decrease.
The number of asteroids decreases markedly with size. Although this generally follows a
power law, there are 'bumps' at 5 km and 100 km, where more asteroids than expected from a
logarithmic distribution are found.
[35]
Approximate number of asteroids N larger than diameter D
| D |
100 m |
300 m |
500 m |
1 km |
3 km |
5 km |
10 km |
30 km |
50 km |
100 km |
200 km |
300 km |
500 km |
900 km |
| N |
~25,000,000 |
4,000,000 |
2,000,000 |
750,000 |
200,000 |
90,000 |
10,000 |
1,100 |
600 |
200 |
30 |
5 |
3 |
1 |
Largest asteroids
Although their location in the asteroid belt excludes them from planet status, the four largest objects,
Ceres,
Vesta,
Pallas, and
Hygiea, are remnant
protoplanets that share many characteristics common to planets, and are atypical compared to the majority of "potato"-shaped asteroids.
| Attributes of protoplanetary asteroids |
| Name |
Orbital
radius (AU) |
Orbital period
(years) |
Inclination
to ecliptic |
Orbital
eccentricity |
Diameter
(km) |
Diameter
(% of Moon) |
Mass
(×1018 kg) |
Mass
(% of Ceres) |
Density[38]
g/cm3 |
Rotation
period
(hr) |
Axial tilt |
Surface
temperature |
| Vesta |
2.36 |
3.63 |
7.1° |
0.089 |
573×557×446
(mean 525) |
15% |
260 |
28% |
3.44 ± 0.12 |
5.34 |
29° |
85–270 K |
| Ceres |
2.77 |
4.60 |
10.6° |
0.079 |
975×975×909
(mean 952) |
28% |
940 |
100% |
2.12 ± 0.04 |
9.07 |
≈ 3° |
167 K |
| Pallas |
2.77 |
4.62 |
34.8° |
0.231 |
580×555×500
(mean 545) |
16% |
210 |
22% |
2.71 ± 0.11 |
7.81 |
≈ 80° |
164 K |
| Hygiea |
3.14 |
5.56 |
3.8° |
0.117 |
530×407×370
(mean 430) |
12% |
87 |
9% |
2.76 ± 1.2 |
27.6 |
≈ 60° |
164 K |
Ceres is the only asteroid large enough for its gravity to force it
into a spheroidal shape, and so, according to the IAU's 2006 resolution
on the
definition of a planet, it has been classified as a
dwarf planet.
[39] Vesta may eventually be so classified as well. Ceres has a much higher
absolute magnitude than the other asteroids, of around 3.32,
[40] and may possess a surface layer of ice.
[41] Like the planets, Ceres is differentiated: it has a crust, a mantle and a core.
[41] Vesta, too, has a differentiated interior, though it formed inside the Solar System's
frost line, and so is devoid of water;
[42] its composition is mainly of basaltic rock such as olivine.
[43] Pallas is unusual in that, like
Uranus, it rotates on its side, with its axis of rotation tilted at high angles to its orbital plane.
[44] Its composition is similar to that of Ceres: high in carbon and silicon, and perhaps partially differentiated.
[45] Hygiea is a carbonaceous asteroid and, unlike the other largest asteroids, lies relatively close to the
plane of the ecliptic.
[46]
Rotation
Measurements of the rotation rates of large asteroids in the asteroid
belt show that there is an upper limit. No asteroid with a diameter
larger than 100 meters has a rotation period smaller than 2.2 hours. For
asteroids rotating faster than approximately this rate, the inertia at
the surface is greater than the gravitational force, so any loose
surface material would be flung out. However, a solid object should be
able to rotate much more rapidly. This suggests that most asteroids with
a diameter over 100 meters are
rubble piles formed through accumulation of debris after collisions between asteroids.
[47]
Composition
Cratered terrain on 4 Vesta
The physical composition of asteroids is varied and in most cases
poorly understood. Ceres appears to be composed of a rocky core covered
by an icy mantle, where Vesta is thought to have a
nickel-iron core,
olivine mantle, and basaltic crust.
[48] 10 Hygiea, however, which appears to have a uniformly primitive composition of
carbonaceous chondrite,
is thought to be the largest undifferentiated asteroid. Most of the
smaller asteroids are thought to be piles of rubble held together
loosely by gravity, though the largest are probably solid. Some
asteroids have
moons or are co-orbiting
binaries: Rubble piles, moons, binaries, and scattered
asteroid families are believed to be the results of collisions that disrupted a parent asteroid.
Asteroids contain traces of
amino acids
and other organic compounds, and some speculate that asteroid impacts
may have seeded the early Earth with the chemicals necessary to initiate
life, or may have even brought life itself to Earth. (See also
panspermia.)
[49] In August 2011, a report, based on
NASA studies with
meteorites found on
Earth, was published suggesting
DNA and
RNA components (
adenine,
guanine and related
organic molecules) may have been formed on asteroids and
comets in
outer space.
[50][51][52]
Composition is calculated from three primary sources:
albedo,
surface spectrum, and density. The last can only be determined
accurately by observing the orbits of moons the asteroid might have. So
far, every asteroid with moons has turned out to be a rubble pile, a
loose conglomeration of rock and metal that may be half empty space by
volume. The investigated asteroids are as large as 280 km in diameter,
and include
121 Hermione (268×186×183 km), and
87 Sylvia (384×262×232 km). Only half a dozen asteroids are
larger than 87 Sylvia,
though none of them have moons; however, some smaller asteroids are
thought to be more massive, suggesting they may not have been disrupted,
and indeed
511 Davida,
the same size as Sylvia to within measurement error, is estimated to be
two and a half times as massive, though this is highly uncertain. The
fact that such large asteroids as Sylvia can be rubble piles, presumably
due to disruptive impacts, has important consequences for the formation
of the Solar system: Computer simulations of collisions involving solid
bodies show them destroying each other as often as merging, but
colliding rubble piles are more likely to merge. This means that the
cores of the planets could have formed relatively quickly.
[53]
On October 7, 2009, the presence of
water ice was confirmed on the surface of
24 Themis using
NASA’s
Infrared Telescope Facility. The surface of the asteroid appears completely covered in ice. As this
ice layer is
sublimated, it may be getting replenished by a reservoir of ice under the surface. Organic compounds were also detected on the surface.
[54][55][56][57] Scientists hypothesize that some of the first water brought to
Earth was delivered by asteroid impacts after the collision that produced the
Moon. The presence of ice on 24 Themis supports this theory.
[56]
Surface features
Most asteroids outside the big four (Ceres, Pallas, Vesta, and
Hygiea) are likely to be broadly similar in appearance, if irregular in
shape. 50-km
253 Mathilde
(shown at right) is a rubble pile saturated with craters with diameters
the size of the asteroid's radius, and Earth-based observations of
300-km
511 Davida,
one of the largest asteroids after the big four, reveal a similarly
angular profile, suggesting it is also saturated with radius-size
craters.
[58] Medium-sized asteroids such as Mathilde and
243 Ida that have been observed up close also reveal a deep
regolith
covering the surface. Of the big four, Pallas and Hygiea are
practically unknown. Vesta has compression fractures encircling a
radius-size crater at its south pole but is otherwise a
spheroid.
Ceres seems quite different in the glimpses Hubble has provided, with
surface features that are unlikely to be due to simple craters and
impact basins, but details will not be known until
Dawn arrives in 2015.
Color
Asteroids become darker and redder with age due to
space weathering.
[59]
However evidence suggests most of the color change occurs rapidly, in
the first hundred thousands years, limiting the usefulness of spectral
measurement for determining the age of asteroids.
[60]
Classification
Asteroids are commonly classified according to two criteria: the
characteristics of their orbits, and features of their reflectance
spectrum.
Orbital classification
Many asteroids have been placed in groups and families based on their
orbital characteristics. Apart from the broadest divisions, it is
customary to name a group of asteroids after the first member of that
group to be discovered. Groups are relatively loose dynamical
associations, whereas families are tighter and result from the
catastrophic break-up of a large parent asteroid sometime in the past.
[61] Families have only been recognized within the
asteroid belt. They were first recognized by
Kiyotsugu Hirayama in 1918 and are often called
Hirayama families in his honor.
About 30% to 35% of the bodies in the asteroid belt belong to
dynamical families each thought to have a common origin in a past
collision between asteroids. A family has also been associated with the
plutoid
dwarf planet Haumea.
Quasi-satellites and horseshoe objects
Some asteroids have unusual
horseshoe orbits that are co-orbital with the
Earth or some other planet. Examples are
3753 Cruithne and
2002 AA29. The first instance of this type of orbital arrangement was discovered between
Saturn's moons
Epimetheus and
Janus.
Sometimes these horseshoe objects temporarily become
quasi-satellites for a few decades or a few hundred years, before returning to their earlier status. Both Earth and
Venus are known to have quasi-satellites.
Such objects, if associated with Earth or Venus or even hypothetically
Mercury, are a special class of
Aten asteroids. However, such objects could be associated with outer planets as well.
Spectral classification
This picture of
433 Eros
shows the view looking from one end of the asteroid across the gouge on
its underside and toward the opposite end. Features as small as 35 m
(115 ft) across can be seen.
In 1975, an asteroid
taxonomic system based on
color,
albedo, and
spectral shape was developed by
Clark R. Chapman,
David Morrison, and
Ben Zellner.
[62]
These properties are thought to correspond to the composition of the
asteroid's surface material. The original classification system had
three categories:
C-types for dark carbonaceous objects (75% of known asteroids),
S-types
for stony (silicaceous) objects (17% of known asteroids) and U for
those that did not fit into either C or S. This classification has since
been expanded to include many other asteroid types. The number of types
continues to grow as more asteroids are studied.
The two most widely used taxonomies now used are the
Tholen classification and
SMASS classification. The former was proposed in 1984 by
David J. Tholen,
and was based on data collected from an eight-color asteroid survey
performed in the 1980s. This resulted in 14 asteroid categories.
[63]
In 2002, the Small Main-Belt Asteroid Spectroscopic Survey resulted in a
modified version of the Tholen taxonomy with 24 different types. Both
systems have three broad categories of C, S, and X asteroids, where X
consists of mostly metallic asteroids, such as the
M-type. There are also several smaller classes.
[64]
Note that the proportion of known asteroids falling into the various
spectral types does not necessarily reflect the proportion of all
asteroids that are of that type; some types are easier to detect than
others, biasing the totals.
Problems
Originally, spectral designations were based on inferences of an asteroid's composition.
[65]
However, the correspondence between spectral class and composition is
not always very good, and a variety of classifications are in use. This
has led to significant confusion. While asteroids of different spectral
classifications are likely to be composed of different materials, there
are no assurances that asteroids within the same taxonomic class are
composed of similar materials.
At present, the spectral classification based on several coarse
resolution spectroscopic surveys in the 1990s is still the standard.
Scientists cannot agree on a better taxonomic system,
[citation needed]
largely due to the difficulty of obtaining detailed measurements
consistently for a large sample of asteroids (e.g. finer resolution
spectra, or non-spectral data such as densities would be very useful).
Exploration
951 Gaspra is the first asteroid to be imaged in close-up (enhanced color).
Several views of 433 Eros in natural colour
Until the age of
space travel,
objects in the asteroid belt were merely pinpricks of light in even the
largest telescopes and their shapes and terrain remained a mystery. The
best modern ground-based telescopes and the Earth-orbiting
Hubble Space Telescope
can resolve a small amount of detail on the surfaces of the largest
asteroids, but even these mostly remain little more than fuzzy blobs.
Limited information about the shapes and compositions of asteroids can
be inferred from their
light curves
(their variation in brightness as they rotate) and their spectral
properties, and asteroid sizes can be estimated by timing the lengths of
star occulations (when an asteroid passes directly in front of a star).
Radar
imaging can yield good information about asteroid shapes and orbital and
rotational parameters, especially for near-Earth asteroids. In terms of
delta-v and propellant requirements, NEOs are more easily accessible than the Moon.
[66]
The first close-up photographs of asteroid-like objects were taken in 1971 when the
Mariner 9 probe imaged
Phobos and
Deimos, the two small moons of
Mars,
which are probably captured asteroids. These images revealed the
irregular, potato-like shapes of most asteroids, as did later images
from the
Voyager probes of the small moons of the
gas giants.
The first true asteroid to be photographed in close-up was
951 Gaspra in 1991, followed in 1993 by
243 Ida and its moon
Dactyl, all of which were imaged by the
Galileo probe en route to
Jupiter.
The first dedicated asteroid probe was
NEAR Shoemaker, which photographed
253 Mathilde in 1997, before entering into orbit around
433 Eros, finally landing on its surface in 2001.
Other asteroids briefly visited by spacecraft en route to other destinations include
9969 Braille (by
Deep Space 1 in 1999), and
5535 Annefrank (by
Stardust in 2002).
In September 2005, the Japanese
Hayabusa probe started studying
25143 Itokawa in detail and was plagued with difficulties, but
returned samples of its surface to earth on June 13, 2010.
The European
Rosetta probe (launched in 2004) flew by
2867 Šteins in 2008 and
21 Lutetia, the second-largest asteroid visited to date, in 2010.
In September 2007,
NASA launched the
Dawn Mission, which orbited the
protoplanet 4 Vesta from July 2011 to September 2012, and is planned to orbit
1 Ceres in 2015. 4 Vesta is the largest asteroid visited to date.
On 13 December 2012, China's lunar orbiter
Chang'e 2 flew within 2 miles (3 km) of the asteroid
4179 Toutatis on an extended mission.
The Japan Aerospace Exploration Agency (JAXA) plans to launch around 2015 the improved
Hayabusa 2 space probe and to return asteroid samples by 2020. Current target for the mission is the
C-type asteroid (162173) 1999 JU3.
In May 2011, NASA announced the
OSIRIS-REx sample return mission to asteroid
1999 RQ36, and is expected to launch in 2016.
It has been suggested that asteroids might be used as a source of materials that may be rare or exhausted on earth (
asteroid mining), or materials for constructing
space habitats (see
Colonization of the asteroids). Materials that are heavy and expensive to launch from earth may someday be mined from asteroids and used for
space manufacturing and construction.
Fiction
Asteroids and the asteroid belt are a staple of science fiction
stories. Asteroids play several potential roles in science fiction: as
places human beings might colonize, resources for extracting minerals,
hazards encountered by spaceships traveling between two other points,
and as a threat to life on Earth by potential impact.
Two Orionids and Milky Way
Multi-colored Orionid
Orionid
The brightest meteor, a fireball, leaves a smoky, persistent trail drifting in high-altitude winds, which is seen at the right-hand side of the image left by Orionid.
A photograph of a Leonids meteor showing a meteor, its afterglow, and its wake
A fireball seen over the desert of Central Australia. Although this occurred during the Lyrids, its North-East entry angle indicates it is sporadic.
Looking down from the International Space Station at a meteor as it passes through the atmosphere
First meteor photographed from Mars, March 7, 2004, by MER Spirit
A sequence of Galileo images, taken several seconds apart, showing the appearance of the fireball of fragment W on the dark side of Jupiter
Willamette Meteorite, discovered in the US state of Oregon
Meteorite, which fell in Wisconsin in 1868.
Murnpeowie meteorite, a thumbprinted iron meteorite.
Marília Meteorite, a chondrite H4, which fell in Marília, São Paulo state, Brazil, on October 5, 1971, at 17:00
Meteorite is from the NWA 869 strewn field, near Tindouf, Algeria. Classified as a L5 COMMON CHONDRITE it shows brecciation and carbon inclusions.[63]
