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Jupiter is more massive than all of the other planets in the solar system combined, plus their satellites,
the asteroids, and all the comets! A mini solar system unto itself. It consists almost entirely of Hydrogen and Helium like
our sun. Jupiter is attended by four of the biggest moons in the solar system, the Galilean satellites Io, Europa, Ganymede,
and Callisto, all of which are larger than Pluto, plus a veritable swarm of other tiny moonlets. Jupiter's deep
gaseous atmosphere merges into a layer of liquid hydrogen. Within the planet pressure and temperature are so high that there
is no clear boundary between the gas and liquid. The atmosphere is composed primarily of hydrogen and helium in nearly the
same abundances found in the Sun and other stars. This enormous planet rotates faster than any other in the solar system,
so fast that its shape is noticeably flattened out of a sphere. The banded and colorful atmosphere contains many gigantic
oval-shaped storms. One of these, the Great Red Spot, is larger than two Earths and has persisted in Jupiter's atmosphere
at least since the 1700s. The atmosphere is probably a few hundred miles in depth, pulled toward the surface by the intense
gravity. Closer to the surface, the gases become more dense, and likely turn into a compound of slurry. Jupiter's rocky
core lies well below the "surface" and is very hot (around 36,000 degrees F.) due to gravitational compression (compression
is a heating process). But Jupiter is much too small and cool to ignite nuclear fusion reactions which are required
to become a star. Jupiter's extremely fast rotation flattens the globe at the poles and drives extremely changeable
weather patterns in the clouds which envelope the planet. The clouds are likely made of ammonia ice crystals, changing
to ammonia droplets further down. It is estimated that the temperature of the cloud tops are about -280 degrees F.
Overall, Jupiter's average temperature is -238 degrees F. Since Jupiter is only tilted slightly more then 3 degrees
on its axis, seasonal fluctuations are minimal. Jupiter is basically a turbulent, stormy, whirlpool of wind, banded
with variable belts and a giant "Red Spot." This giant Red Spot is an oval shaped, counter-clockwise
moving storm and is four times larger than our Earth. The storm is by far the largest of similar ovals found on other
parts of Jupiter and the other gas giants. Jupiter's wind appears to be driven by internal heat rather than from solar
insolation. Jupiter was the first target for Pioneers 10 and 11 in 1972 and 1973 and Voyagers 1 and 2 in 1979.
From 1995 to 2003, the Galileo orbiter toured the Jupiter system. Jupiter's mass makes it an attractive waypoint for gravity
assist trajectories, which allow spacecraft to reach otherwise inaccessible points in the solar system. The solar orbiter
Ulysses in 1992 and Saturn orbiter Cassini in 2000 took advantage of Jupiter gravity assists. The Pluto mission New Horizons
will be the next spacecraft to fly by Jupiter in February 2007. The gas planets do not have solid surfaces, their
gaseous material simply gets denser with depth (the radii and diameters quoted for the planets are for levels corresponding
to a pressure of 1 atmosphere). What we see when looking at these planets is the tops of clouds high in their atmospheres
(slightly above the 1 atmosphere level). Jupiter is about 90% hydrogen and 10% helium (by numbers of atoms, 75/25% by mass)
with traces of methane, water, ammonia and "rock". This is very close to the composition of the primordial Solar
Nebula from which the entire solar system was formed. Saturn has a similar composition, but Uranus and Neptune have much less
hydrogen and helium. Our knowledge of the interior of Jupiter (and the other gas planets) is highly indirect and likely to
remain so for some time. (The data from Galileo's atmospheric probe goes down only about 150 km below the cloud tops.) Jupiter
probably has a core of rocky material amounting to something like 10 to 15 Earth-masses.
Above the core lies the main bulk of the planet
in the form of liquid metallic hydrogen. This exotic form of the most common of elements is possible only at pressures exceeding
4 million bars, as is the case in the interior of Jupiter (and Saturn). Liquid metallic hydrogen consists of ionized protons
and electrons (like the interior of the Sun but at a far lower temperature). At the temperature and pressure of Jupiter's
interior hydrogen is a liquid, not a gas. It is an electrical conductor and the source of Jupiter's magnetic field. This layer
probably also contains some helium and traces of various "ices". The outermost layer is composed primarily of ordinary
molecular hydrogen and helium which is liquid in the interior and gaseous further out. The atmosphere we see is just the very
top of this deep layer. Water, carbon dioxide, methane and other simple molecules are also present in tiny amounts. Recent
experiments have shown that hydrogen does not change phase suddenly. Therefore the interiors of the jovian planets probably
have indistinct boundaries between their various interior layers. Three distinct layers of clouds are believed to exist consisting
of ammonia ice, ammonium hydrosulfide and a mixture of ice and water. However, the preliminary results from the Galileo probe
show only faint indications of clouds (one instrument seems to have detected the topmost layer while another may have seen
the second). But the probe's entry point (left) was unusual -- Earth-based telescopic observations and more recent observations
by the Galileo orbiter suggest that the probe entry site may well have been one of the warmest and least cloudy areas on Jupiter
at that time. Data from the Galileo atmospheric probe also indicate that there is much less water than expected. The expectation
was that Jupiter's atmosphere would contain about twice the amount of oxygen (combined with the abundant hydrogen to make
water) as the Sun. But it now appears that the actual concentration much less than the Sun's. Also surprising was the high
temperature and density of the uppermost parts of the atmosphere. Jupiter and the other gas planets have high velocity
winds which are confined in wide bands of latitude. The winds blow in opposite directions in adjacent bands. Slight chemical
and temperature differences between these bands are responsible for the colored bands that dominate the planet's appearance.
The light colored bands are called zones; the dark ones belts. The bands have been known for some time on Jupiter, but the
complex vortices in the boundary regions between the bands were first seen by Voyager. The data from the Galileo probe indicate
that the winds are even faster than expected (more than 400 mph) and extend down into as far as the probe was able to observe;
they may extend down thousands of kilometers into the interior. Jupiter's atmosphere was also found to be quite turbulent.
This indicates that Jupiter's winds are driven in large part by its internal heat rather than from solar input as on Earth.
The vivid colors seen in Jupiter's clouds are probably the result of subtle chemical reactions of the trace elements in Jupiter's
atmosphere, perhaps involving sulfur whose compounds take on a wide variety of colors, but the details are unknown. The colors
correlate with the cloud's altitude: blue lowest, followed by browns and whites, with reds highest. Sometimes we see the lower
layers through holes in the upper ones. The Great Red Spot (GRS) has been seen by Earthly observers for more than 300
years (its discovery is usually attributed to Cassini, or Robert Hooke in the 17th century). The GRS is an oval about 12,000
by 25,000 km, big enough to hold two Earths. Other smaller but similar spots have been known for decades. Infrared observations
and the direction of its rotation indicate that the GRS is a high-pressure region whose cloud tops are significantly higher
and colder than the surrounding regions. Similar structures have been seen on Saturn and Neptune. It is not known how such
structures can persist for so long. Jupiter radiates more energy into space than it receives from the Sun.
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The interior of Jupiter is hot: the core is probably about 20,000 K. The
heat is generated by the Kelvin-Helmholtz mechanism, the slow gravitational compression of the planet. (Jupiter does NOT produce
energy by nuclear fusion as in the Sun; it is much too small and hence its interior is too cool to ignite nuclear reactions.)
This interior heat probably causes convection deep within Jupiter's liquid layers and is probably responsible for the complex
motions we see in the cloud tops. Saturn and Neptune are similar to Jupiter in this respect, but oddly, Uranus is not. Jupiter
is just about as large in diameter as a gas planet can be. If more material were to be added, it would be compressed by gravity
such that the overall radius would increase only slightly. A star can be larger only because of its internal (nuclear) heat
source. (But Jupiter would have to be at least 80 times more massive to become a star.) Jupiter has a huge magnetic field,
much stronger than Earth's. Its magnetosphere extends more than 650 million km (past the orbit of Saturn!). (Note that Jupiter's
magnetosphere is far from spherical -- it extends "only" a few million kilometers in the direction toward the Sun.)
Jupiter's moons therefore lie within its magnetosphere, a fact which may partially explain some of the activity on Io. Unfortunately
for future space travelers and of real concern to the designers of the Voyager and Galileo spacecraft, the environment near
Jupiter contains high levels of energetic particles trapped by Jupiter's magnetic field. This "radiation" is similar
to, but much more intense than, that found within Earth's Van Allen belts. It would be immediately fatal to an unprotected
human being. The Galileo atmospheric probe discovered a new intense radiation belt between Jupiter's ring and the uppermost
atmospheric layers. This new belt is approximately 10 times as strong as Earth's Van Allen radiation belts. Surprisingly,
this new belt was also found to contain high energy helium ions of unknown origin. Jupiter has rings like Saturn's, but much
fainter and smaller (right). They were totally unexpected and were only discovered when two of the Voyager 1 scientists insisted
that after traveling 1 billion km it was at least worth a quick look to see if any rings might be present. Everyone else thought
that the chance of finding anything was nil, but there they were. It was a major coup. They have since been imaged in the
infra-red from ground-based observatories and by Galileo. Unlike Saturn's, Jupiter's rings are dark (albedo about .05). They're
probably composed of very small grains of rocky material. Unlike Saturn's rings, they seem to contain no ice. Particles in
Jupiter's rings probably don't stay there for long (due to atmospheric and magnetic drag). The Galileo spacecraft found clear
evidence that the rings are continuously resupplied by dust formed by micrometeor impacts on the four inner moons, which are
very energetic because of Jupiter's large gravitational field. The inner halo ring is broadened by interactions with Jupiter's
magnetic field. In July 1994, Comet Shoemaker-Levy 9 collided with Jupiter with spectacular results (left). The effects were
clearly visible even with amateur telescopes. The debris from the collision was visible for nearly a year afterward with HST.
When it is in the nighttime sky, Jupiter is often the brightest "star" in the sky (it is second only to Venus, which
is seldom visible in a dark sky). The four Galilean moons are easily visible with binoculars; a few bands and the Great Red
Spot can be seen with a small astronomical telescope. There are several Web sites that show the current position of Jupiter
(and the other planets) in the sky. More detailed and customized charts can be created with a planetarium program. Jupiter
has 63 known satellites (as of Feb 2004): the four large Galilean moons plus many more small ones some of which have not yet
been named:
Jupiter is very gradually slowing down due to the tidal drag produced
by the Galilean satellites. Also, the same tidal forces are changing the orbits of the moons, very slowly forcing them farther
from Jupiter. Io, Europa and Ganymede are locked together in a 1:2:4 orbital resonance and their orbits evolve together. Callisto
is almost part of this as well. In a few hundred million years, Callisto will be locked in too, orbiting at exactly twice
the period of Ganymede (eight times the period of Io). Jupiter's satellites are named for other figures in the life of Zeus
(mostly his numerous lovers). Many more small moons have been discovered recently but have not as yet been officially confirmed
or named. The most up to date info on them can be found at Scott Sheppard's site.
Jupiter (Click on photo's
to enlarge)
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Jupiter Size: largest planet - 142,984 kilometers diameter - 11.21 Earths across Calendar: 1 Jupiter year = 11.857 Earth years; 1 Jupiter day = 0.414 Earth days Orbit: 778,570,000 kilometers - 5.204
Earth orbits Average distance from Sun 482,300,000 miles Perihelion 459,100,000 miles Aphelion 506,300,000
miles Sidereal Rotation 9.925 Earth hours Length of Day 9.925 Earth hours Sidereal Revolution 11.87 Earth
years Diameter at Equator 88,650 miles (largest planet) Tilt of axis 3.13 degrees Moons 63 known Atmosphere
Hydrogen (90%), Helium (10%), trace amounts of methane and ammonia Discoverer Unknown Discovery Date Prehistoric
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