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Io biography, Io discography
Io
Jupiter I
Nothing endures but change.It is the most volcanic body known, with lava flows,
lava lakes, and giant calderas covering its
sulfurous landscape.It has billowing volcanic geysers spewing
sulfurous plumes to over 500 kilometers high.Its mountains are
much taller than those on Earth,
reaching heights of 16 kilometers (52,000 feet).Io orbits closer to Jupiter's cloud tops than the
moon does to Earth.This places Io within an intense radiation belt that bathes the
satellite with energetic electrons, protons, and heavier ions.As
the Jovian magnetosphere
rotates, it sweeps past Io and strips away
about 1,000 kilograms (1 ton) per second of volcanic gases and other
materials.This produces a neutral cloud of atoms orbiting with Io as
well as a huge, doughnut shaped torus of ions that glow in the
ultraviolet.The torus's heavy ions migrate outward, and their
pressure inflates the Jovian magnetosphere to more than twice its
expected size.Some of the more energetic sulfur and oxygen ions fall
along the magnetic field into the planet's atmosphere, resulting in
auroras.Io acts as an electrical generator as it moves through Jupiter's magnetic
field, developing 400,000 volts across its diameter and generating an
electric current of 3 million amperes that flows along the magnetic field
to the planet's
ionosphere.Above Auroral Glow:
This eerie view of Io was acquired by the Galileo spacecraft while the moon
was in Jupiter's shadow.The vivid colors
are caused by
collisions between Io's atmospheric gases and energetic charged particles
trapped in Juiter's magnetic field.The green and red emissions are
probably produced by mechanisms similar to those in Earth's polar regions
that produce aurora.Bright blue glows mark the sites of dense plumes
of volcanic vapor, and may be places where Io is electrically connected
to Jupiter.Io Discoveries
On January 7, 1610 Galileo Galilei observed three pinpoints of light
strung out in a line next to Jupiter.After a week, Galileo observed that
the four stars never left the vicinity of Jupiter, appeared to be
carried along with the planet, and changed their position with
respect to each other and Jupiter.Finally, Galileo determined that what
he was observing were not stars, but planetary bodies that were in orbit
around Jupiter.This discovery provided evidence in support of the still
heretical Copernican solar system and showed that everything did not
revolve around the Earth.Simon de Laplace during the late 1700s when he deduced
that the orbital periods of Io, Europa, and Ganymede are nearly in a
perfect 1:2:4 ratio.These in turn were used to calculate the
mean density of Io (3.Left: This cutaway illustration shows the possible internal structure of Io.The interior characteristics of the moon are inferred from gravity field and
magnetic field measurements by the Galileo spacecraft.Io has a metallic (iron, nickel)
core (shown in gray) drawn to the correct relative size.The core is surrounded
by a rock shell (shown in brown).Io's rock or silicate shell extends to the surface.Based on density, surface composition analysis, and gravity data, Io
appears to be a rocky silicate rich body that has a dense iron, iron
sulfide core that extends halfway to the surface with a partially melted
silicate rich mantle, and a thin rocky crust.During the early formation of the
solar system,
Jupiter would have been very hot.This may have prevented lighter
elements from condensing at the inner orbits.The mini system of Galilean
satellites orbiting Jupiter resembles that of the solar system with the
rocky, dense planets at the innermost orbits and the light, least dense
planets at the outer orbits.Galileo Galilei
Date of discovery1610
Mass (kg)8.Mean distance from Jupiter (km)421,600
Rotational period (days)1.Io Rotation with Enhanced Colors.This color image of Io was created by combining the color
channels of the low resolution USGS Voyager controlled color mosaic with
Tayfun Oner's high resolution Galileo mosaic.Mountainous regions exist near both poles, with some
features rising 8 kilometers (5 miles) or more above their surroundings.This is the highest resolution color global mosaic of Io.It was then projected to an ortographic projection
centered at 0 degrees latitude and 315 degrees longitude.For comparison, the
photo on the left was taken in March 1994 before the spot emerged,
and shows that Io's surface had undergone only subtle changes since it
was last seen by the Voyager 2 probe in 1979.The new spot in the July 1995 Hubble image replaces a smaller whitish
spot seen at about the same location in the March 1994 image."The new
spot surrounds the volcano Ra Patera, which was photographed by Voyager,
and is probably composed of material, probably frozen gas, ejected from
Ra Patera by a large volcanic explosion or fresh lava flows,"
according to John Spencer of Lowell Observatory in Flagstaff, Arizona.Voyager 2 took this picture of Io
on the evening of July 9, 1979, from a range of 1.On the limb of Io are two blue volcanic eruption
plumes about 100 kilometers (62 miles) high.They apparently had been erupting for a period of at
least four months and probably longer.Voyager 2, all of which were first seen by Voyager 1.Plume 4 was not viewed on the edge of Io's disc by Voyager 2
and, therefore, it is not known whether it was still erupting.This image is the highest resolution image ever taken of Io.Illumination is from the lower right, but the topographic
shading is difficult to see because of the strong contrasts in
brightness of the surface materials.The bright areas are generally
higher in elevation than adjacent dark areas.Evaporation of solid ice may also play a role
in separating the bright and dark materials.This is a close up view of Io's northern hemisphere.The central feature has been named Loki Patera.This photograph of Io shows what
appears to be a volcanic caldera that is venting gasses (the bright blue
patch at left center).Io, it is
possible that sulfur dioxide is the main component of the clouds.Sulfur
dioxide clouds would rapidly freeze and snow back to the surface.It is
also possible that dark areas in the floors of the calderas are pools of
molten sulfur, a very dark form of sulfur.The image was taken March 5,
1979, as Voyager 1 approached Io, and was taken from
129,600 kilometers (80,500 miles).The
volcanic eruption can be seen on the limb of Io.Ra Patera is a large shield volcano with multi colored flows.Io is slightly larger than Earth's Moon.The pronunciation "EE oh" is also acceptable.Io has a core of iron (perhaps mixed with iron sulfide)
with a radius of at least 900 km.Io's surface is radically different from any other body in the solar system.But there are very few, if any, impact craters on Io (left).The material erupting from Io's vents appears to be some form of sulfur or
sulfur dioxide.The volcanic eruptions change rapidly.Ra Patera has also been seen by
HST.These observations confirm that Io's surface is very active indeed.Sulfur and its compounds take on a wide range of colors which are
responsible for Io's variegated appearance.One current idea is that Io's
lavas are molten silicate rock.Or there may be a variety of different materials in different locations.Some of the
hottest spots
on Io may reach temperatures as high as 2000 K though the average is much lower,
about 130 K.These hot spots are the principal mechanism
by which Io loses its heat.The energy for all this activity probably derives from tidal interactions
between Io, Europa, Ganymede and Jupiter.Europa which in turn orbits twice for each orbit of
Ganymede.This wobbling stretches and bends
Io by as much as 100 meters (a 100 meter tide!Moon is not heated by Earth in this way.Io also cuts across Jupiter's magnetic field lines, generating an
electric current.Though small compared to the tidal heating, this
current may carry more than 1 trillion watts.Io which forms a torus of intense radiation
around Jupiter.Recent data from Galileo indicate that Io may have its own magnetic field as does Ganymede.Io has a thin atmosphere composed of sulfur dioxide and perhaps some other
gases.Unlike the other Galilean satellites, Io has little or no water.It seems that Io is radiating heat faster than the tidal mechanism can
generate it.Or is there some
additional source of heat?What mechanism drives the volcanoes?Does Io have its own magnetic field?Express to Europa
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serialization, which lets a program write whole objects out to streams
and read them back again.Then the lesson looks at some file system
operations, including random access files.Most of the classes covered are in the java.Buffered Streams optimize input
and output by reducing the number of calls to the native API.Scanning and Formatting allows
a program to read and write formatted text.Standard Streams and the Console object.Summary
A summary of the key points covered in this trail.Questions and Exercises
Test what you've learned in this trail by trying these questions and exercises.The example programs contained in these lessons are standalone
applications, which by default have no security manager.See
Security Restrictions for information about the security restrictions placed on applets.
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