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First Planet From the Sun

Mean distance from the Sun: 57.9 million kilometers

Mean orbital velocity: 47.89 kilometers per second

Length of mercurian year: 0.2408 Earth-year, 87.9 Earth-days

Length of mercurian day: 58.6 Earth-days

Diameter: 4,878 kilometers

Mass: 0.0558 Earth-mass

Number of known satellites: 0

Once Mercury was thought to be the littlest, hottest planet, and scientists believed that it kept one face always toward the Sun. Spacecraft, radar and telescopic observations have disproved those erstwhile "facts;" they have also revealed new mysteries about this small world closest to the Sun. While Pluto is the littlest and Venus is the hottest, Mercury is the densest planet, with its interior dominated by a huge iron core. Evidently the core is partly molten, since it must act like a dynamo to generate Mercury's weak, but Earthlike, magnetic field. It is surprising that the core's heat has not all leaked into space through Mercury's thin mantle; it is also difficult to fathom dynamo action inside such a slowly rotating body (Mercury's spin is exactly two-thirds of its 88-day orbital year).

Scientists once thought Mercury to be nearly a carbon-copy of our Moon, but that's not true! Gently rolling intercrater plains distinguish its surface and its surface reflectivity is different. Mercury is unique in being crisscrossed by enormous thrust faults formed as the planet contracted while it cooled. Although Mercury's atmosphere - perhaps related to the solar wind sometimes reaching the planet's surface - is tenuous, many scientists were surprised that Mercury has any atmosphere at all.

In many ways, Mercury is at out near the end of the spectrum of planetary properties: in solar distance, composition, dynamical properties, size and environmental conditions. It is a fascinating, if inhospitable planet, difficult to glimpse from Earth as it hides in the Sun's glare, but available for follow-up studies by technically advanced, heat-resistant spacecraft .- Clark R. Chapman, Planetary Science Institute, Science Applications International Corporation

This mosaic view of Mercury was produced from images taken by the Mariner 10 spacecraft on the outbound leg of its first flyby of the planet in March, 1974. The planet's north pole is at the top and its equator extends from left to right, about two-thirds down from the top.

The Mariner 10 mission to Venus and Mercury was the first space mission to demonstrate the gravity-assist technique: using the motion and gravity of one planet to alter a spacecraft's trajectory and send it to another planet.

Image processing: JPL/NASA. Mosaiking: United States Geological Survey 2-VENUS Image

Second Planet From the Sun

Distance from the Sun: 108.2 million kilometers

Mean orbital velocity: 35.03 kilometers per second

Length of venusian year: 0.6152 Earth-years, 225 Earth-days

Length of venusian day: 243 Earth-days

Diameter: 12,100 kilometers

Mass: 0.8150 Earth-mass

Number of known satellites: 0

Venus has often been called Earth's sister world, for the two planets are about the same size and orbit in the same neighborhood of the solar system. But spacecraft and Earth-based investigations have revealed Venus as a very different world. The planet rotates about its axis in a retrograde direction (opposite to its orbital direction) and its day is equal to 243 Earth-days, longer than its year.

Venus's thick atmosphere is composed of carbon dioxide, with clouds of sulfuric acid. Winds in the atmosphere rotate about the planet in only four Earth-days, despite the slow rotation of the surface. The surface pressure on Venus is about 90 times that on Earth, and the temperature is 500 degrees Celsius (900 degrees Fahrenheit). This high temperature is due to the "greenhouse effect:" short-w0opd[d[avelength (visible) light is able to penetrate the thick atmosphere, but longer-wavelength radiation emitted by the warmed planet is absorbed by the blanket of carbon dioxide. This causes the temperature to increase until the amount of the heat that can "leak" from the planet comes into equilibrium with the solar energy received. - Robert Papalardo, Planetary Geology Group, Arizona State University

This mini-poster displays a false-color global view of Venus' western hemisphere as seen by Magellan's synthetic aperture radar. To create this image, radar mosaics from Magellan's first mapping cycle were laid over a computer-simulated globe.

The bright, twisted feature that undulates horizontally across the globe is the equatorial highland Aphrodite Terra. The volcano Maat Mons lies on its eastern end, to the right of center. To the lower left, in Aphrodite Terra, lies Artemis Corona, a circular feature 2,600 kilometers (about 1,600 miles) in diameter. Many other smaller coronae are also visible across the surface. Coronae, first identified in the data returned from the Soviet Venera 15 and 16 spacecraft, are thought to form due to the upwelling of plumes of hot material from deep within the interior of the planet. They probably spread out, cool and subside, resulting in the typical collapsed bubble appearance.

Impact craters can be found in many places on Venus' surface. Look for small, crisp circular features, frequently surrounded by a dark patch. These result from meteorites blasting through the atmosphere and striking the surface at high velocity. The dark splotches that surround many of the craters probably result from interaction with the thick atmosphere as the meteor hurtled toward the surface. There are many well-preserved large impact craters which probably date back about 800 years.

Image: JPL/NASA 3-EARTH Image

Third Planet From the Sun

Mean distance from the Sun: 149.6 million kilometers

Mean orbital velocity: 29.79 kilometers per second

Length of terrestrial year: 365.256 Earth-days

Length of terrestrial day: 1 Earth-day

Diameter: 12,756 kilometers

Mass: 1 Earth-mass

Number of known satellites: 1

Earth, the planet of blue water, is our home. Alone in the solar system, it possesses a robust living skin called the biosphere. Living things have been on Earth for at least 3.5 of the 4.5 billion years of the planet's history, and this life has profoundly influenced the chemistry, geology and climate of Earth.

Our planet's great beauty and color came into sharp focus with the first viewing of Earth from space in the late 1960s. This shift in perception has stimulated scientific awareness of the interconnection among the geology, the atmosphere, the great oceans and the living organisms that affect and are affected by these physical systems. Truly, the history of Earth without the biosphere would have produced a very different world from the one we see today.

The presence of free oxygen and the chemical and oxidation state of many other gases in the atmosphere are directly due to the activities of life. These substances, in turn, affect the temperature and climate of Earth through mechanisms like the "greenhouse effect," which may cause global warming. The ocean's chemistry results from the complex interaction of inorganic geological processes and biological activities that produce many compounds unique to life.

The vast quantity of liquid water on the planet and the remarkable activity of plate tectonics greatly affected the origin of life and its evolution on Earth. The continents move over the planet's surface, changing the currents and climates of the land. This has alternately separated and brought together countless different kinds of organisms under myriad conditions. Indeed, the combination of all these properties may have been requisite for the diversity of life on Earth.

We are only just beginning to catch a tantalizing glimpse of the complex choreography of life on a planet. We are on the threshold of major leaps in understanding of the workings of our home planet. This is very exciting time to be an inhabitant of the lovely planet, Earth. - Penelope J. Boston, Complex Systems Research.

Galileo captured this view of Earth's partially illuminated Australasian hemisphere on December 9, 1992. This image was taken 31 hours after the spacecraft's closest approach to the planet during its second flyby. In this false-color composite, vegetation appears red so that even small islands like Tasmania can be seen to the south of Australia, along with cloud-covered New Guinea and the Solomon Islands to the north.

Image: Paul Geissler, Lunar and Planetary Laboratory, University of Arizona 4-MARS Image

Fourth Planet From the Sun

Mean distance from the Sun: 227.9 million kilometers

Mean orbital velocity: 24.13 kilometers per second

Length of martian year: 1.881 Earth-year

Length of martian day: 1.02 Earth-days

Diameter: 6,786 kilometers

Mass: 0.1074 Earth-mass

Number of known satellites: 2

Mars is more like Earth than any other object in our solar system, although it is only half as large. It has mountains and valleys, volcanos and earthquake faults, dry river beds and polar ice caps. It has an atmosphere with clouds, winds and dust storms. It has summer and winter seasons. Its surface is solid and composed mainly silicon dioxide (sand). And its temperature is moderate by astronomical, if not human, standards. Consequently, it is the only place beyond the Moon that we can seriously consider visiting.

The contrasts are more striking than the similarities, however. Because its crust is very thick and rigid, there is no continental drift on Mars and there are no mountain ranges like the Sierras or the Himalayas. But volcanos erupting over billions of years have built up mountains that dwarf any on Earth. Its polar caps are composed mainly of carbon dioxide ice, but the northern cap evaporates in the summer, leaving a smaller cap containing only water ice.

The atmosphere is about 95 percent carbon dioxide, with nitrogen and argon next in abundance. Its pressure and density are about 100 times less than on Earth, and they fluctuate by about 30 percent with the seasonal waxing and waning of the polar caps. Mars receives less than half the intensity of sunlight as Earth and, primarily because of its meager and transparent atmosphere, it is a very cold place. In summer the air temperature never gets up to the melting point of water ice, and in winter it often falls to the freezing point of carbon dioxide, minus180 degrees Fahrenheit. Being so cold, the atmosphere cannot hold much water vapor, even though the lower levels are often saturated. As it never rains, the presence of many dry river beds, both large and small, is one of the major mysteries of Mars.

The composition of the soil is about one-fifth ferric oxide - rusty iron - which accounts for the red color of both the surface and the sky.

For scientists in many fields, Mars is a fascinating laboratory. Meteorologists are interested in the modes of atmospheric circulation that don't occur on Earth. Geologists are interested in the composition and structure of the interior, the way surface features have formed and are still evolving. Biologists are interested in whether any primitive life-forms ever existed, and if not, why not. Some of these questions may be solved by remotely controlled spacecraft in the next decade or two, but others will have to wait for people to walk on the surface sometime in the next century. - Conway Snyder, Jet Propulsion Laboratory

This mosaic of the Schiaparelli hemisphere of Mars is composed of about 100 Viking Orbiter images, creating a view very similar to that which one might see from a spacecraft. The images were taken in 1980 during Mars' northern summer at a distance of about 2,500 kilometers (1,550 miles) from the planet's surface. Schiaparelli is the large impact crater near the center of the globe. The color variations in this image have been enhanced by a factor of two, and the bright areas to the south are covered with carbon dioxide frost.

Image: United States Geological Survey, Flagstaff, Arizona 5-JUPITER Image

Fifth Planet From the Sun

Mean distance from the Sun: 778.3 million kilometers

Mean orbital velocity: 13.06 kilometers per second

Length of jovian year: 11.86 Earth-years

Length of jovian day: 0.41 Earth-day

Diameter: 142,796 kilometers

Number of known satellites: 16

Jupiter is aptly named for the king of the gods in the Greco-Roman pantheon. This planet is more massive than all of the others combined, plus their satellites, the asteroids and all the comets. Jupiter has 16 known satellites, and the largest, Ganymede, is bigger than the planet Mercury. The planet's magnetic field is so powerful that it creates a sphere of influence around Jupiter that is larger than the Sun. As if all this were not enough, the Voyager spacecraft discovered that the planet has a tenuous ring system and that its Moon-sized satellite lo is wracked by volcanism far more intense than any we find on our own planet.

Even in a small telescope, Jupiter is distinguished by bands of clouds that change their appearance over time. More remarkable is a persistent pattern of winds that have lasted for the many decades that the planet has been observed from Earth. The huge oval storm known as the Great Red Spot has persisted for at least 300 years.

Jupiter's atmosphere is composed primarily of hydrogen and helium in nearly the same abundances that we find in the Sun and other stars. The expected hydrogen-dominated compounds methane (CH4), water (H20) and ammonia (NH) have all been found, but we've also seen unanticipated compounds, acetylene (C2H2), carbon monoxide (CO) and hydrogen cyanide (HCN), for example. These substances are formed by ultraviolet light from the Sun, lighting discharges within the clouds and the internal heat escaping from the planet.

The composition of the clouds is still a mystery. The white ones are almost certainly ammonia cirrus, but a variety of pale pastels, mainly variations in yellow and brown with some salmon and blue-gray patches, indicates that chemical reactions are producing colored substances from the main gaseous constituents. Sulfur compounds are the likely sources of such colors, but no firm identification has yet been made.

Jupiter's deep gaseous atmosphere merges imperceptibly 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. Closer to Jupiter's center, the pressure becomes high enough to squeeze electrons out of the hydrogen atoms so they can move freely through the liquefied gas as they do in metals. Jupiter's intense magnetic field is generated within this highly conducting layer of metallic hydrogen.

The wealth of phenomena on display at Jupiter invites us to return again to learn more about the fundamental physical and chemical processes that have produced the planets and shaped their environments.- Tobias Owen, University of Hawaii, Honolulu

This picture of Jupiter was taken by Voyager 2 on May 9, 1979 from a distance of about 46 million kilometers (almost 29 million miles). A similar image captured by Voyager 1 about four months earlier revealed to scientists that the planet's atmosphere undergoes constant change, presenting an ever-shifting face to observers.

Image: JPL/NASA 6-SATURN Image

Sixth Planet From the Sun

Mean distance from the Sun: 1,427 million kilometers

Mean orbital velocity: 9.64 kilometers per second

Length of saturnian year: 29.46 Earth-years

Length of saturnian day: 0.43 Earth-day

Diameter: 120,000 kilometers

Mass: 95 Earth-masses Number of known satellites: 18

Ever since 1610 when Galileo first looked at Saturn through a telescope, the planet has been distinguished by its prominent ring system. Now that we have traveled to Saturn with our spacecraft we realize the full significance of this miniature planetary system.

Saturn is one of the gas giants in our solar system. It's comprised mainly of hydrogen gas, with a diameter about 10 times that of Earth. Stretching from nearly the outer atmosphere of the planet to the middle of the satellite system, the rings are made up of countless small particles ranging in size from dust to mountain-sized masses. The thickest part of the ring system, easily seen in photographs of the planet, looks like a grooved phonograph record and is made up of hundreds of individual features. We now know that these features are caused by the gravitational forces from Saturn's moons orbiting nearby.

The study of these features not only has revealed information about the rings and moons of Saturn, but also about the physics of disks of material. This knowledge is being applied to other planetary ring systems, to the study of the formation of planets around other stars, and even to our understanding of the spiral structure of galaxies. The saturnian system of planet, moons and rings has provided a laboratory for the study of many planetary and astrophysical problems.

Beside these important scientific contributions gained by their study, the rings of Saturn are also one of the most awesome and beautiful sights in our solar system. So widespread is the recognition of the rings of Saturn that their image has come to represent a universal symbol for "outer space." - Richard Terrile, Jet Propulsion Laboratory

In 1981 the Voyager 2 spacecraft captured this image of Saturn and its vast system of rings. Three of the planet's small icy moons are also visible, along with the shadow of a fourth.

Image: JPL/NASA. 7-URANUS Image

Seventh Planet From the Sun

Mean distance from the Sun: 2,875 million kilometers

Mean orbital velocity: 6.8 kilometers per second

Length of uranian year: 84 Earth-years

Length of uranian day: 17.24 hours, 0.79 Earth-day

Equatorial diameter: 51,100 kilometers

Mass: 14.54 Earth-masses

Number of known satellites: 15

A remarkable thing about Uranus is that its axis is almost in its orbital plane - that is, the planet is tilted onto its side. More remarkable yet, the orbits of its five major moons are tilted the same way. The magnetic axis does not share this regularity: It is midway between the pole and equator - the greatest tilt known for any planet. Like Jupiter and Saturn, the surface, if any, is buried at enormous depths; all we can see is atmosphere and clouds. The atmosphere is mostly hydrogen and helium, but it's at least 10 times richer in methane (CH4) than those of Jupiter and Saturn; Voyager 2 even observed a dense methane cloud layer. If there are other clouds of ammonia (NH3) or water (H2O), they too are deeply buried.

The spidery ring system was discovered in 1978 as Uranus passed over (occulted) a star, and many occultations have been observed since then. The proposal that individual planetary rings are confined by "shepherding moons" arose from these results; later this idea was applied to the detail in the saturnian rings found by the Voyagers. Voyager 2 found a very extended corona, or outermost atmosphere, of hydrogen atoms enveloping the uranian rings. This medium must exert large drag forces on ring particles and cause them to spiral into the atmosphere, just like a re-entering satellite. Many workers believe that the rings we see are temporary, having been formed by a collision between unknown moonlets in the last few million years.- D.M. Hunten, University of Arizona

Other collisions are evident in the tiny moon Miranda, which was very well-photographed by Voyager 2. Its incredibly patchy surface is the result of episodic partial melting of the moon's interior, during which heavier rocky materials sank and viscous water ice rose toward the surface forming the features known as coronae. The heat source may be a combination of radioactive material accreted with Miranda as it formed and tidal heating from earlier times when Miranda's orbit was more elliptical. As it passed through orbital resonances with the other uranian moons, their gravities may have tugged on the tiny moon, heating it up. - E.D. Miner, Jet Propulsion Laboratory

As the Voyager 2 spacecraft departed from the uranian system, it looked back and snapped this farewell shot of the crescent planet on January 25, 1986 from a distance of about 965,600 kilometers (600,000 miles).

Image: JPL/NASA 8-NEPTUNE Image

Eighth Planet From the Sun

Mean distance from the Sun: 4,500 million kilometers

Mean orbital velocity: 5.4 kilometers per second

Length of neptunian year: 164.8 Earth-years

Length of neptunian day: 16.11 hours, 0.67 Earth-day

Equatorial diameter: 49,500 kilometers

Mass: 17.15 Earth-masses

Number of known satellites: 8

Neptune is over 50 percent farther from the Sun than its near twin in size and appearance, Uranus, but its temperature is equal to or slightly greater than that of Uranus. Its internal energy is such that it emits nearly 2.5 times as much energy as it receives from the Sun. The escaping internal energy may also power the storms and winds in Neptune's atmosphere, which are the fastest in the solar system. Like the other gas giant planets, Neptune probably has no solid surface. The planet's observable atmosphere is primarily hydrogen and helium, and it owes its beautiful blue color to an abundance of methane in its atmosphere, which absorbs red light and reflects blue. High clouds of methane ice cast shadows on deeper, possibly ammonia, ice crystal clouds.

Earth-based observations had hinted at a system of broken rings, or arcs, around Neptune, but Voyager 2s images revealed a sparse but continuous ring system. Neptune's outermost ring has three dense areas. The next ring in is also narrow but without denser ring arc regions. Two broad inner regions of ring material complete the neptunian ring system. The rings are embedded in a magnetic field tilted 50 degrees to Neptune's equator and offset from the center of the planet by more than half of its radius.

Voyager 2 added six small moons to Neptune's known retinue, all relatively close to the planet. Tiny Nereid, the outermost moon, occupies the most eccentric orbit of any moon in the solar system. But Triton is the most curious of Neptune's satellites. It is the only large moon in the solar system to orbit "backwards" around its planet. Voyager 2 found Triton to have a tenuous nitrogen atmosphere, the coldest surface temperatures in the solar system, an enormous polar cap of nitrogen ice and active geyser-like plumes erupting through the ice cap. Triton may well be a Pluto-like object, formed independently of Neptune in the outer solar system but later "captured" by the planet's gravity. - E.D. Miner, Jet Propulsion Laboratory

This portrait of Neptune was captured when Voyager 2 flew past the planet in August, 1989. Three of the planet's most prominent atmospheric features are visible in this picture reconstructed from two Voyager 2 images. From top (north) to bottom is the large storm system known as the Great Dark Spot, the bright, rapidly-rotating "Scooter" and farther south is the "Dark Spot 2" with its bright core.

Five years later, in 1994, two independent teams of scientists discovered that these atmospheric features had disappeared. The researchers, from the Jet Propulsion Laboratory and the Massachusetts Institute of Technology, studied Neptune with the Hubble Space Telescope and found an almost featureless disk. The new studies show that the giant planet's atmosphere undergoes dramatic changes in just a few months, or even a week's time.

Image: JPL/NASA 9-PLUTO Image

Ninth Planet From the Sun

Mean distance from the Sun: 5,900 million kilometers

Mean orbital velocity: 4.7 kilometers per second

Length of plutonic year: About 248.5 Earth-years

Length of plutonic day: 6.4 Earth-days

Mass: About 0.0022 Earth-mass

Number of known satellites: 1

Discovered in 1930 by Clyde Tombaugh from the Lowell Observatory in Flagstaff, Arizona, Pluto is the most recently discovered planet. It is the only planet that will not be visited by spacecraft during the 20th century and so, for some time to come, Pluto will remain the most enigmatic planet. Because Pluto is smaller than Earth's Moon and orbits at a tremendous distance from the Sun, it is only a bright speck in the strongest telescopes.

Unlike the other planets that orbit beyond Mars - the gas giants - Pluto is small, with only a very thin atmosphere, composed mainly of methane (CH4) gas, and it orbits the Sun in a steeply inclined and eccentric orbit. For about 20 Earth-years out of each 248.5-year orbit, Pluto is actually closer to the Sun than is Neptune. Pluto will be traversing this part of its orbit between 1980 and 1999. It passed perihelion (its closest approach to the Sun) in 1989.

Pluto is practically a double planet. Its satellite, Charon (discovered in 1978 by James Christy of the US Naval Observatory), is the largest satellite relative to its parent planet in the solar system. Charon's diameter of some 1,200 kilometers is about half that of Pluto, and it orbits its planet at a distance of about 17 Pluto radii. In contrast, our Moon's diameter is about one-quarter of Earth's, which it orbits at a distance of about 60 Earth radii. Like Pluto, Charon may also have a thin atmosphere, but we have not yet determined its composition.

Charon's orbital period is equal to Pluto's rotation period, so the length of a plutonic day and month are the same. Because of this, to a person standing on Pluto directly under Charon the satellite would appear to remain stationary, forever hanging over that spot. Conversely, a person on the diametrically opposite side of Pluto would never see the satellite at all!

Pluto's surface is covered with methane ice, while Charon's is covered with water ice. This strange pair, locked in distant orbit, will be an extremely intriguing target for exploratory spacecraft in what we hope will be the not-too-distant future - Edward F. Tedesco, Jet Propulsion Laboratory

Pluto was the first solar system object to be imaged by the Hubble Space Telescope. The European Space Agency's Faint Object Camera aboard the telescope captured this first distinct view ever of Pluto and Charon, its large moon. Charon appears fainter here, not only because it is smaller than Pluto, but because its surface is covered with water ice, whereas Pluto is believed to be covered mainly by more reflective methane frost or snow.

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