Solar System, the Sun and everything
that orbits the Sun, including the planets and their satellites; the dwarf
planets, asteroids, Kuiper Belt Objects, and comets; and interplanetary dust
and gas. The term may also refer to a group of celestial bodies orbiting
another star (see Extrasolar Planets). In this article, solar system
refers to the system that includes Earth and the Sun.
The dimensions of the solar system are
specified in terms of the mean distance from Earth to the Sun, called the
astronomical unit (AU). One AU is 150 million km (about 93 million mi).
Estimates for the boundary where the Sun’s magnetic field ends and interstellar
space begins—called the heliopause—range from 86 to 100 AU from the Sun.
The most distant known body orbiting
the Sun is the dwarf planet Eris, whose discovery was reported in July 2005.
Eris is currently about 97 AU from the Sun. Another planetlike object in the
outer solar system named Sedna is currently at 90 AU but will reach about 900
AU at the farthest point in its orbit thousands of years from now. Comets known
as long-period comets, however, achieve the greatest distance from the Sun;
they have highly eccentric orbits ranging out to 50,000 AU or more. (A comet’s
period is how long it takes it to complete one revolution about the Sun.) They
are members of the Oort cloud, a spherical shell of comet nuclei that surrounds
the flat plane of planetary orbits at this enormous distance.
The solar system was the only
planetary system known to exist around a star similar to the Sun until 1995,
when astronomers discovered a planet about 0.6 times the mass of Jupiter
orbiting the star 51 Pegasi. Jupiter is the most massive planet in our solar
system. Soon after, astronomers found a planet about 8.1 times the mass of
Jupiter orbiting the star 70 Virginis, and a planet about 3.5 times the mass of
Jupiter orbiting the star 47 Ursa Majoris. Since then, astronomers have found
planets and disks of dust in the process of forming planets around many other
stars. Most astronomers think it likely that solar systems of some sort are
numerous throughout the universe. See Astronomy; Galaxy; Star.
II
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THE SUN AND THE
SOLAR WIND
|
The Sun is a typical star of
intermediate size and luminosity. Sunlight and other radiation are produced by
the conversion of hydrogen into helium in the Sun’s hot, dense interior (see
Nuclear Energy). Although this nuclear fusion is transforming 600 million
metric tons of hydrogen each second, the Sun is so massive (2 × 1030
kg, or 4.4 × 1030 lb) that it can continue to shine at its present
brightness for 6 billion years. This stability has allowed life to develop and
survive on Earth.
For all the Sun’s steadiness, it
is an extremely active star. On its surface, dark sunspots bounded by intense
magnetic fields come and go in 11-year cycles and sudden bursts of charged
particles from solar flares can cause auroras and disturb radio signals on
Earth. A continuous stream of protons, electrons, and ions also leaves the Sun
and moves out through the solar system. This solar wind shapes the ion tails of
comets and leaves its traces in the lunar soil, samples of which were brought
back from the Moon’s surface by piloted United States Apollo spacecraft (see
Space Exploration; Apollo program).
The Sun’s activity also influences the
heliopause, a region of space that astronomers believe marks the boundary
between the solar system and interstellar space. The heliopause is a dynamic
region that expands and contracts due to the constantly changing speed and
pressure of the solar wind. In November 2003 a team of astronomers reported
that the Voyager 1 spacecraft appeared to have encountered the outskirts of the
heliopause at about 86 AU from the Sun. They based their report on data that
indicated the solar wind had slowed from 1.1 million km/h (700,000 mph) to
160,000 km/h (100,000 mph). This finding is consistent with the theory that
when the solar wind meets interstellar space at a turbulent zone known as the
termination shock boundary, it will slow abruptly. However, another team of
astronomers disputed the finding, saying that the spacecraft had neared but had
not yet reached the heliopause.
III
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THE MAJOR PLANETS
|
Eight major or classical planets are
currently recognized by the International Astronomical Union (IAU), the body that
gives official names to objects in the solar system. The planets are commonly
divided into two groups: the inner planets (Mercury, Venus, Earth, and Mars)
and the outer planets (Jupiter, Saturn, Uranus, and Neptune). The inner planets
are small and are composed primarily of rock and iron. The outer planets are
much larger and consist mainly of hydrogen, helium, and ice. Pluto,
historically counted as the ninth planet, does not belong to either group, and
was reclassified as a dwarf planet by the IAU in 2006. Some astronomers have
objected to the reclassification of Pluto and the new IAU definition of a
planet. Others feel strongly that classifying Pluto as one of the largest
members of a family of similar icy bodies orbiting the Sun beyond Neptune provides
a much better explanation of Pluto’s existence.
The IAU has defined a classical
planet as a body that orbits the Sun, that has a rounded shape from the effects
of its own gravity, and that is the dominant object in its region of space and
has cleared the neighborhood of its orbit of other objects. A dwarf planet is
also a rounded body orbiting the Sun—but one that is not massive enough to have
cleared its region of space of other objects.
Mercury is surprisingly dense, apparently
because it has an unusually large iron core. With only a transient atmosphere,
Mercury has a surface that still bears the record of bombardment by asteroidal
bodies early in its history. Venus has a carbon dioxide atmosphere 90 times
thicker than that of Earth, causing an efficient greenhouse effect by which the
Venusian atmosphere is heated. The resulting surface temperature is the hottest
of any planet—about 477°C (about 890°F).
Earth is the only planet known to
have abundant liquid water and life. However, in 2004 astronomers with the
National Aeronautics and Space Administration’s Mars Exploration Rover mission
confirmed that Mars once had liquid water on its surface. Scientists had
previously concluded that liquid water once existed on Mars due to the numerous
surface features on the planet that resemble water erosion found on Earth.
Mars’s carbon dioxide atmosphere is now so thin that the planet is dry and
cold, with polar caps of frozen water and solid carbon dioxide, or dry ice.
However, small jets of subcrustal water may still erupt on the surface in some
places.
Jupiter is the largest of the planets.
Its hydrogen and helium atmosphere contains pastel-colored clouds, and its
immense magnetosphere, rings, and satellites make it a planetary system unto
itself. One of Jupiter’s largest moons, Io, has volcanoes that produce the
hottest surface temperatures in the solar system. At least four of Jupiter’s
moons have atmospheres, and at least three may contain liquid or partially
frozen water. Jupiter’s moon Europa may have a global ocean of liquid water
beneath its icy crust.
Saturn rivals Jupiter, with a much more
intricate ring structure and a similar number of satellites. One of Saturn’s
moons, Titan, has an atmosphere thicker than that of any other satellite in the
solar system. Another moon of Saturn, Enceladus, has liquid-water geysers.
Uranus and Neptune are deficient in hydrogen compared with Jupiter and Saturn;
Uranus, also ringed, has the distinction of rotating at 98° to the plane of its
orbit. See also Planetary Science.
IV
|
OTHER ORBITING
BODIES
|
Three dwarf planets are currently
recognized by the IAU: Pluto, Eris, and Ceres. Astronomers may designate more
dwarf planets in the near future. Pluto and Eris are dwarf planets according to
the IAU because they have rounded shapes from their own gravity but have not
cleared their neighborhoods in space of other objects—both orbit through the
Kuiper Belt, a region beyond Neptune containing thousands of small icy bodies.
Pluto and Eris are composed of layers of ice around a rocky core. Ceres
qualifies as a dwarf planet because it is spherical but is found in the
asteroid belt, a zone between the orbits of Mars and Jupiter that contains
thousands of small rocky bodies. Ceres is likely made up of a rocky core
surrounded by a mantle containing a mix of rock and ice. Like asteroids, dwarf
planets are listed by the IAU as minor planets with numbers and names.
The asteroids are small, rocky bodies
that move in orbits primarily between the orbits of Mars and Jupiter. Numbering
in the thousands, asteroids range in size from around 530 km (329 mi)—about
half the size of the dwarf planet Ceres—to microscopic grains. Some asteroids
are perturbed, or pulled by forces other than their attraction to the Sun, into
eccentric orbits that can bring them closer to the Sun. If the orbits of such
bodies intersect that of Earth, they are called meteoroids. When they appear in
the night sky as streaks of light, they are known as meteors, and recovered
fragments are termed meteorites. Laboratory studies of meteorites have revealed
much information about primitive conditions in our solar system. The surfaces
of Mercury, Mars, and several satellites of the planets (including Earth’s
moon) show the effects of an intense bombardment by asteroidal and cometary
objects early in the history of the solar system. On Earth that record has
eroded away, except for a few recently found impact craters.
Some meteors and interplanetary dust
may also come from comets, which are basically aggregates of dust and frozen
gases typically 5 to 10 km (about 3 to 6 mi) in diameter. Comets orbit the Sun
at distances so great that they can be perturbed by stars into orbits that
bring them into the inner solar system. As comets approach the Sun, they
release their dust and gases to form a spectacular coma and tail. Under the
influence of Jupiter’s strong gravitational field, comets can sometimes adopt
much smaller orbits. The most famous of these is Halley’s Comet, which returns
to the inner solar system at 75-year periods. Its most recent return was in
1986. In July 1994 fragments of Comet Shoemaker-Levy 9 bombarded Jupiter’s
dense atmosphere at speeds of about 210,000 km/h (130,000 mph). Upon impact,
the tremendous kinetic energy of the fragments was released through massive
explosions, some resulting in fireballs larger than Earth.
Comets circle the Sun in two main
groups, within the Kuiper Belt or within the Oort cloud. The Kuiper Belt is a
disk of icy debris that orbits the Sun beyond the planet Neptune. The
population of the Kuiper Belt is made up of Kuiper Belt Objects (KBOs). KBOs
range in size from clumps of ice mixed with rock dust (“dirty snowballs”) up to
dwarf planets such as Pluto and Eris. Any of these icy objects could be
considered a comet nucleus that would give off gas and dust to produce a coma
and a tail if its orbit were to bring it close enough to the Sun. Most of the
comets with periods of less than 500 years come from the Kuiper Belt.
The Oort cloud is a hypothetical
region about halfway between the Sun and the heliopause. Astronomers believe
that the existence of the Oort cloud, named for Dutch astronomer Jan Oort,
explains why some comets have very long periods. A chunk of dust and ice may
stay in the Oort cloud for thousands of years. Nearby stars sometimes pass
close enough to the solar system that their gravitational force will push an
object in the Oort cloud into an orbit that takes it close to the Sun.
The first detection of the
long-hypothesized Oort cloud came in March 2004 when astronomers reported the
discovery of a planetoid about 1,700 km (about 1,000 mi) in diameter. They
named it Sedna, after a sea goddess in Inuit mythology. Sedna was found about
13 billion km (about 8 billion mi) from the Sun. At its farthest point from the
Sun, Sedna is the most distant object in the solar system and is about 130
billion km (about 84 billion mi) from the Sun.
Many of the objects that do not
fall into the asteroid belts, the Kuiper Belt, or the Oort cloud may be comets
that will never make it back to the Sun. The surfaces of the icy satellites of
the outer planets are scarred by impacts from such bodies. The asteroid-like
object Chiron, with an orbit between Saturn and Uranus, may itself be an
extremely large inactive comet. Similarly, some of the asteroids that cross the
path of Earth’s orbit may be the rocky remains of burned-out comets. Chiron and
similar objects called the Centaurs probably escaped from the Kuiper Belt and
were drawn into their irregular orbits by the gravitational pull of the giant
outer planets, Jupiter, Saturn, Neptune, and Uranus.
The Sun was also found to be
encircled by rings of interplanetary dust. One of them, between Jupiter and
Mars, has long been known as the cause of zodiacal light, a faint glow that
appears in the east before dawn and in the west after dusk. Another ring, lying
only two solar widths away from the Sun, was discovered in 1983.
V
|
MOVEMENTS OF THE
PLANETS AND THEIR SATELLITES
|
If one could look down on the
solar system from far above the North Pole of Earth, the planets would appear
to move around the Sun in a counterclockwise direction. All of the planets
except Venus and Uranus, and the dwarf planet Pluto, rotate on their axes in
this same direction. The entire system is remarkably flat—only Mercury among
the major planets has an obviously inclined orbit. However, the dwarf planets
Pluto and Eris have orbits that are strongly tilted out of the main plane of
the solar system, Pluto at 17.2° and Eris at 44°. Both objects also have highly
elliptical orbits. Pluto’s orbit sometimes takes it closer than Neptune to the
Sun. At its nearest point to the Sun, Eris passes inside the orbit of Pluto,
though well beyond the orbit of Neptune.
The satellite systems mimic the behavior of
their parent planets and move in a counterclockwise direction, but many
exceptions are found. Jupiter, Saturn, Uranus, and Neptune each have a number
of satellites that move around the planet in a retrograde orbit (clockwise
instead of counterclockwise), and several satellite orbits are highly
elliptical. Uranus has some satellites that follow its clockwise direction and
others that move in counterclockwise orbits. Jupiter, moreover, has trapped two
clusters of planetesimals or small rocky bodies (the so-called Trojan
asteroids) leading and following the planet by 60° in its orbit around the Sun.
Neptune also has groups of planetesimals that share its orbit. (Some satellites
of Saturn have done the same with smaller bodies that occupy different parts of
the same orbits as the satellites.) The long-period comets exhibit a roughly
spherical distribution of orbits around the Sun, while most of the short-period
comets appear to originate from the disklike distribution of Kuiper Belt
Objects.
Within this maze of motions, some
remarkable patterns exist: Mercury rotates on its axis three times for every
two revolutions about the Sun; no asteroids exist with periods 1/2, 1/3, … 1/n
(where n is an integer) the period of Jupiter; the three inner Galilean
satellites of Jupiter have periods in the ratio 4:2:1. Some Kuiper Belt Objects
(including Pluto) orbit the Sun in a 2:3 ratio to Neptune’s orbit. These and
other examples demonstrate the subtle balance of forces that is established in
a gravitational system composed of many bodies.
VI
|
THEORIES OF ORIGIN
|
Despite their differences, the members of
the solar system probably form a common family. They seem to have originated at
the same time; few indications exist of bodies joining the solar system,
captured later from other stars or interstellar space.
Early attempts to explain the origin of
this system include the nebular hypothesis of the German philosopher Immanuel
Kant and the French astronomer and mathematician Pierre Simon de Laplace,
according to which a cloud of gas broke into rings that condensed to form
planets. Doubts about the stability of such rings led some scientists to
consider various catastrophic hypotheses, such as a close encounter of the Sun
with another star. Such encounters are extremely rare, and the hot, tidally
disrupted gases would dissipate rather than condense to form planets.
Current theories connect the formation of
the solar system with the formation of the Sun itself, about 4.6 billion years
ago. The fragmentation and gravitational collapse of an interstellar cloud of
gas and dust, triggered perhaps by nearby supernova explosions, may have led to
the formation of a primordial solar nebula. The Sun would then form in the
densest, central region. It is so hot close to the Sun that even silicates,
which are relatively dense, have difficulty forming there. This phenomenon may
account for the presence near the Sun of a planet such as Mercury, having a
relatively small silicate crust and a larger than usual, dense iron core. (It
is easier for iron dust and vapor to coalesce near the central region of a
solar nebula than it is for lighter silicates to do so.) At larger distances
from the center of the solar nebula, gases condense into solids such as are
found today from Jupiter outward. Evidence of a possible preformation supernova
explosion appears as traces of anomalous isotopes in tiny inclusions in some
meteorites. This association of planet formation with star formation suggests
that billions of other stars in our galaxy may also have planets. The high
frequency of binary and multiple stars, as well as the large satellite systems
around Jupiter and Saturn, attest to the tendency of collapsing gas clouds to
fragment into multibody systems.
The formation of our solar system
may have been an even more complex process than once thought. Recent studies of
the chemistry of comets based on NASA’s Deep Impact and Stardust missions
indicate that such primitive objects contain a surprising mix of materials that
formed in both the hot inner regions and the cold outer regions of the early
solar system. Some computer models show that the giant planets may have formed
closer to the Sun, then moved outward over time, changing the orbits of other
planets. Other models suggest inward migration of Jupiter and Saturn, imitating
the orbital histories of some giant extrasolar planets that have been found
orbiting very close to their parent stars. Our early solar system likely
contained additional planets that were either destroyed in collisions with other
planets or were thrown out of the solar system completely. The study of solar
systems around other stars promises to provide important additional insights.
See separate articles for most of the
celestial bodies mentioned in this article. See also Exobiology.
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