<text>Jupiter statisticsDistance from the Sun Maximum: 505.7 millions miles 815.7 millions km 5.455 AU Minimum: 459.4 millions miles 740.9 millions km 4.951 AU Mean: 482.6 millions miles 778.3 millions km 5.203 AUPeriod of revolution ("one year"): 11.86 yearsPeriod of rotation (equatorial): 9 hr. 50 min. 30 sec.Mean orbital velocity per second: 8.1 miles (13.1 km)Inclination of axis: 3.1°Orbital eccentricity: 0.048Orbital inclination: 1.31°Diameter at equator: 89,424 miles 143,884 km 11.2 x Earth's diameterOblateness: 0.064Escape velocity per second: 37.0 miles (59.5 km)Mean surface temperature: -238 F / -150 C / 123° K (at cloud tops)Mass 1.9 x 10^30 kg (Earth = 1): 318Volume (Earth =1): 1,319Density (water = 1): 1.33Surface gravity: 22.9 m/s^2 (Earth = 1): 2.64Maximum apparent diameter as seen from Earth (seconds of arc): 50".1Mean diameter of Sun as seen from the planet: 6' 09"Albedo: 0.44Number of knwon satellites: 16Satellite dataMetisMean distance from center of planet: 79,530 mi. (127,960 km)Orbital period: 0.295 daysOrbital eccentricity: 0Orbital inclination to planet's equator: 0°Diameter: 25 mi. (40 km)Escape velocity: 0.010? mph (0.02? kph)Magnitude: 17.4Maximum apparent diameter as seen from the planet: unknownAdrasteaMean distance from center of planet: 80,160 mi. (128,980 km)Orbital period: 0.298 daysOrbital eccentricity: 0Orbital inclination to planet's equator: 0°Diameter: 16 x 12 x 10 mi. (26 x 20 x 16 km)Escape velocity: 0.006? mph (0.01? kph)Magnitude: 18.9Maximum apparent diameter as seen from the planet: ---AmaltheaMean distance from center of planet: 112,680 mi. (181,300 km)Orbital period: 0.498 daysOrbital eccentricity: 0.003Orbital inclination to planet's equator: 0.45°Diameter: 163 x 91 x 83 mi. (262 x 146 x 134 km)Escape velocity: 0.010? mph (0.16? kph)Magnitude: 14.1Maximum apparent diameter as seen from the planet: 7' 24"ThebeMean distance from center of planet: 137,900 mi. (221,900 km) Orbital period: 0.675 daysOrbital eccentricity: 0.013Orbital inclination to planet's equator: 0.9°Diameter: 68 x 62 x 56 mi. (110 x 100 x 90 km)Escape velocity: 0.006? mph (0.1? kph)Magnitude: 15.5Maximum apparent diameter as seen from the planet: unknownIoMean distance from center of planet: 262,030 mi. (421,600 km)Orbital period: 1.769 daysOrbital eccentricity: 0.004Orbital inclination to planet's equator: 0.04°Diameter: 2, 264 mi. (3,642 km)Escape velocity: 1.590 mph (2.56 kph)Magnitude: 5.0Maximum apparent diameter as seen from the planet: 35' 40"EuropaMean distance from center of planet: 416,970 mi. (670,900 km) Orbital period: 3.551 daysOrbital eccentricity: 0.009Orbital inclination to planet's equator: 0.47°Diameter: 1,945 mi. (3,130 km)Escape velocity: 1.310 mph (2.10 kph)Magnitude: 5.3Maximum apparent diameter as seen from the planet: 17' 30"GanymedeMean distance from center of planet: 665,000 mi. (1.,070,000 km) Orbital period: 7.155 daysOrbital eccentricity: 0.002Orbital inclination to planet's equator: 0.21°Diameter: 3,274 mi. (5,268 km)Escape velocity: 1.730 mph (2.78 kph)Magnitude: 4.6Maximum apparent diameter as seen from the planet: 18' 06"CallistoMean distance from center of planet: 1,168,400 mi. (1,880,000 km)Orbital period: 16.689 days Orbital eccentricity: 0.007Orbital inclination to planet's equator: 0.51°Diameter: 2,987 mi. (4,806 km)Escape velocity: 1.510 mph (2.43 kph)Magnitude: 5.6Maximum apparent diameter as seen from the planet: 9' 30"LedaMean distance from center of planet: 6,805,000 mi. (11,094,000 km)Orbital period: 238.7 daysOrbital eccentricity: 0.148Orbital inclination to planet's equator: 26.1°Diameter: 6 mi. (10 km)Escape velocity: 0.003? mph (0.005? kph)Magnitude: 20.2Maximum apparent diameter as seen from the planet: 0" .2HimaliaMean distance from center of planet: 7,134,900 mi. (11,480,000 km)Orbital period: 250.6 daysOrbital eccentricity: 0.158Orbital inclination to planet's equator: 27.6°Diameter: 106 mi. (170 km)Escape velocity: 0.060? mph (0.1? kph)Magnitude: 14.8Maximum apparent diameter as seen from the planet: 8" .2LysitheaMean distance from center of planet: 7,284,000 mi. (11,720,000 km)Orbital period: 259.2 daysOrbital eccentricity: 0.107Orbital inclination to planet's equator: 29.0°Diameter: 15 mi. (24 km)Escape velocity: 0.006? mph (0.01? kph)Magnitude: 18.4Maximum apparent diameter as seen from the planet: 0" .1ElaraMean distance from center of planet: 7,295,000 mi. (11,737,000 km)Orbital period: 259.7 daysOrbital eccentricity: 0.207Orbital inclination to planet's equator: 24.8°Diameter: 50 mi. (80 km)Escape velocity: 0.030? mph (0.05? kph)Magnitude: 16.7Maximum apparent diameter as seen from the planet: 1" .4AnankeMean distance from center of planet: 13,176,000 mi. (21,200,000 km)Orbital period: 631 daysOrbital eccentricity: 0.17Orbital inclination to planet's equator: 147°Diameter: 12 mi. (20 km)Escape velocity: 0.006? mph (0.01? kph)Magnitude: 18.9Maximum apparent diameter as seen from the planet: 0" .02?CarmeMean distance from center of planet: 14,046,000 mi. (22,600,000 km)Orbital period: 692 daysOrbital eccentricity: 0.21Orbital inclination to planet's equator : 164°Diameter: 19 mi. (30 km)Escape velocity: 0.010? mph (0.02? kph)Magnitude: 18.0Maximum apparent diameter as seen from the planet: 0" .02?PasiphaÎMean distance from center of planet: 14,605,000 mi. (23,500,000 km)Orbital period: 735 days Orbital eccentricity: 0.38Orbital inclination to planet's equator: 145°Diameter: 22 mi. (36 km)Escape velocity: 0.01? mph (0.02? kph)Magnitude: 17.7Maximum apparent diameter as seen from the planet: 0" .02?SinopeMean distance from center of planet: 14,730,000 mi. (23,700,000 km)Orbital period: 758 daysOrbital eccentricity: 0.28Orbital inclination to planet's equator: 153°Diameter: 17 mi. (28 km)Escape velocity: 0.006? mph (0.01? kph)Magnitude: 18.3Maximum apparent diameter as seen from the planet: 0" .01?Planet compositionJupiter is the largest planet in the solar system. By comparison, Jupiter's volume is 1,330 times greater than Earth, and its mass is 318 times greater. Mass of Jupiter, in fact, accounts for two-thirds of the total mass of all the planets combined.Jupiter's low density suggests that planet is composed of light elements; in particular hydrogen and helium in gas and liquid form. The planet's center is thought to be a small (10 to 20 Earth masses) rocky core of iron and silicates, surrounded by liquid or solid hydrogen. About 1,000 km from the visible surface, researchers believe there is a transition zone from gaseous to liquid hydrogen, where the temperature is about 3,141° F / 1,727° C / 2,000° K and the pressure about 5,600 atm. At 3,000 km below the clouds, the temperature is about 9,451° F / 5,263° C / 5,500° K and the pressure is 90,000 atm. At 25,000 km below the cloud tops, the temperature is over 19,341° F / 10,727° C / 11,000° K and the pressure is about 3,000,000 atm. At this point, hydrogen changes from liquid molecular to liquid metallic hydrogen. Maximum temperatures reach 53,541° F / 29, 727° C / 30,000° K and 100 million atm at the core. Crust: 500 kmMantle: 13,500 - 14,500 kmCore: 46,000 kmTopographyThe most prominent "topographical" feature is the Great Red Spot (16,280 x 8,575 miles). Located in atmosphere over the southern hemisphere, this hurricane-like storm is more than twice the size of Earth. It was perhaps first seen and documented by Robert Hooke in 1664, but researchers believe it may be millions of years old. The Great Red Spot is much colder than its surroundings, with temperatures averaging -202°F. As a high-pressure region, the Great Red Spot spins the opposite direction of low-pressure storms on Jupiter.AtmosphereJupiter's atmosphere is largely hydrogen (<90%) and helium (<10%). Ammonia, methane, ethane, acetylene, water vapor, phosphine, carbon monoxide, germane, and tetrahydride also present in small quantities. By comparison, the basic structure of Jupiter's atmosphere resembles Earth's tropospheric levels.The Jovian magnetosphere is thought to be about 100 times as strong as Earth's and to have areas similar to our Van Allen Belts. The size of Jupiter's magnetosphere changes in response to interaction the solar wind. The collision with solar wind particles forms a shock wave (called a bow shock), within which there is a turbulent region known as a Magnetopause. In this region, Voyager measured temperatures of 602 - 751 million° F / 300-400 million° C / 300-400 million° Kóthe highest found in the solar system.The atmosphere surrounding Jupiter contains dark streaks (known as cloud belts) and bright bands (known as cloud zones). Several of each variety are relatively stable, changing only slightly in latitude. Some occasionally disappear. Ammonia crystals form white clouds in Jupiter's atmosphere, while sulfur compounds (and perhaps phosphorus) produce the brown and orange hues typically associated with Jupiter's appearance. Magnetic fields and gravityResearchers believe that Jupiter's magnetic field is generated by a dynamo. The electrical conductor is believed to be liquid hydrogen at or near the planet's core, but the force driving the system is unknown. (Researchers speculate that it involves planetary rotation.) The magnetic field on Jupiter is inclined to the planet's axis of rotation by an angle of about 11° (as compared to 10∞ on Earth), and the alignment of the magnetic poles is such that a compass needle would point south.On Jupiter, the surface gravity is 2.69.Orbit and rotationJupiter has an elliptical orbit that takes 4,332.59 days (11.86 years) to complete. Because it is mostly fluid, Jupiter's period of rotation varies with latitude, the fastest rotation being at the equator (9 hours 50 minutes 30 seconds). This fast rotation causes a bulge to form, making the planet's equatorial diameter about 142,800 km, while its polar diameter is only 132,400 km.Moons (and/or rings)Jupiter has 16 known satellites. The four largest Io, Europa, Ganymede, and Callistoóare known collectively as the Galileans in honor of the first observer, Galileao Galilei on January 7, 1610. All the Galileans have a synchronous rotation (they orbit Jupiter in the same amount of time it takes to rotate on their axes) and all are the size of planets. Of note, Io has nine active volcanoes, the only such volcanoes known in the solar system (except on Earth).Jupiter is also surrounded by rings, which consist of several segments and seem to extend to the planet's surface. Researchers believe that the are made up of relatively high-density rocks (dust), as opposed to the icy material found in Saturn's rings. They also believe the rings originated from the gravitational break-up of a tiny inner satellites, plus materials from other satellites, comets, and meteorites.MythologyJupiter was named for the ruler of Olympus. Amalthea was named for the one who suckled Zeus (Greek for Jupiter) as a young child. Io was named for the daughter of Inachus. Europa was named for the beautiful daughter of Agenor, king of Tyhre. Ganymede was named for a beautiful young boy who, after being carried to Olympus by Zeus, became cup bearer of the Olympian gods. Callisto was named for the beautiful daughter of Lycaon. Discovery and explorationIn 1972, NASA sent the first of four spacecraft slated to conduct the initial surveys. Pioneer 10 lifted off in March 1972 and returned the first close-up images of Jupiter in December 1973, flying within 132,252 km (82,178 miles) of the cloud tops. Pioneer 11 followed 1 year later. Voyagers 1 and 2 were launched in the summer of 1977 and did flybys in 1979.A new mission to Jupiter, known as the Galileo project, is under way. On December 7, 1995, the orbiter will spend two years circling the planet and flying close to the large moons. It will also drop an atmospheric probe into the cloud layers to relay information back to Earth.</text>
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<text>Venus statisticsDistance from the Sun: Maximum: 67.6 million miles 108.9 million km 0.728 AU Minimum: 66.7 million miles 107.4 million km 0.718 AU Mean: 67.2 million miles 108.2 million km 0.723 AUPeriod of revolution: 224.7 daysPeriod of rotation (equatorial): 243.0 days (retrograde)Mean orbital velocity: 21.8 miles (35 km) per secondInclination of axis: 178 degreesOrbital eccentricity: 0.007Orbital inclination: 3.39 degreesDiameter at equator: 7,523 miles (12,104 km) / 0.949 x EarthΓÇÖs diameterOblateness: 0Mass: 4.87 x 10^24 kg 0.815 x EarthΓÇÖs massVolume: 9.32 x 10^11 km^3 0.86 x EarthΓÇÖs volumeDensity: 5.24 g/cm^3 0.949 x EarthΓÇÖs densitySurface gravity: 8.60 m/s^2 0.90 x EarthΓÇÖs gravityEscape velocity: 6.4 miles (10.4 km) per secondMean surface temperature: 896 F / 480 C / 753 KMaximum apparent diameter as seen from Earth: 65.2ΓÇ¥Albedo: 0.76Number of known moons: 0Mean diameter of Sun as seen from the planet: 44' 15"Planet composition: Researchers believe that Venus, which is almost perfectly spherical, has a liquid iron core smaller than the Earth's. This would be surrounded by a mantle composed of silicates. However, it is possible that Venus does not have a discrete core, and has iron and silicates mixed throughout the planet instead of being separated into a mantle and core. The crust ranges from 25 km thick in the lowlands to 160 km thick in the highlands. This relatively thick static crust may be composed of a single plate. Soil samples taken by Veneras 9 and 10 indicate that Venus' crust has a composition similar to terrestrial ocean deposits.Core: 2800 to 3100 km (radius)Mantle: 3000 km thickCrust: 25 to 160 km thickTopography: The topography of Venus is diverse. A series of large (up to 150 km in diameter) but shallow craters populate the surface. There are also highlands (average elevation of 3 km) and a system of faults. The two large highlands areas are Ishtar Terra, in the northern hemisphere, and Aphrodite Terra, slightly to the south of the equator. Ishtar Terra is about the size of Australia, and its highest point (11 km) occurs in a grouping known as the Maxwell Mountains. Aphrodite Terra is about the size of Africa and its highest point is 7 km. Diana Chasma is Venus' largest valley, lying about 4 km below the surrounding ridges. The largest basin is Atlanta Planitia, which is comparable in size to the Gulf of Mexico.Atmosphere: The atmosphere of Venus is composed primarily of carbon dioxide (96%). The rest is mostly nitrogen, with sulfuric acid, carbon monoxide, oxygen, water vapor, hydrochloric acid, and hydrofluoric acid all present in trace amounts. Venus' atmosphere is so dense that the pressure at the surface is over 90 times greater than on the surface of the Earth. Only at an elevation of 50 km does the pressure reach the Earth's sea-level pressure. The majority of Venusian clouds consist of sulfuric acid droplets which condense at altitudes between 45 and 75 km. They form broad bands in the atmosphere, and their thickness hides the surface of the planet from view. The large amount of carbon dioxide causes an effect known as greenhouse warming: solar energy which is reflected from the Venusian surface is absorbed by the carbon dioxide as well as sulfuric acid. Therefore, heat is trapped within the atmosphere and is distributed across the planet, making the surface extremely hot (896 F / 480 C / 753 K).Magnetic fields and gravity: Though Venus has only a very small magnetic field, it still interacts with the solar wind. An ionosphere is created in Venus' thick atmosphere as high energy solar wind particles collide with and ionize neutral atmospheric atoms and molecules. The ionosphere causes a bow shock on the side of Venus facing the Sun; away from the Sun it extends outwards in a tear-shaped tail. There are many charged particles which constitute the ionosphere, but none of them are magnetically trapped in radiation belts.Gravity: The gravity at the surface of Venus is 0.902 times the Earth's gravity.Orbit and rotation: Venus has the most circular orbit of any planet. Its rotation is also unique: First, it takes longer for the planet to rotate on its axis than it takes to orbit the Sun. (The globe rotation is at the equator is 243 days, whereas the planet's year is only 224.7 days.) Second, Venus rotates east to west, which is retrograde (backward) from that of the Sun and most other planets. Finally, it's interesting to note that Venus' upper atmosphere rotates around the planet in only four days, while the planet itself takes 243 days to complete one revolution.Moons and/or rings: Venus is so bright it sometimes produces a ghost image. Astronomers in the 17th and 18th centuries thought the image to be a satellite, but it has since been confirmed that there are no satellites associated with Venus.Mythology: Venus has been known for centuries. The ancient Babylonians named it Nin-dar-Anna, "Mistress of the Heavens;" the Chinese, Tai-pe, "The Beautiful White One;" the Greeks, Hesperus, the "Evening star," and Phosphorus, the "Morning star." The planet is named for the Roman goddess of love and beauty, and astrologers believed that any child born under the rays of Venus would be blessed with those features. Venus was the symbol of gentleness and charm, a taste for music, harmony, playfulness, and generosity. Friday, in ancient times, was dedicated to Venus.Discovery and exploration: Galileo first viewed Venus close-up using an "optick tube" in 1610. In the eighteenth century, J.H. Schroeter confirmed the existence of an atmosphere. In the nineteenth century, imaginative speculation regarding possible life forms on Venus abounded, fueled by the fictional writings of Jules Verne. Illustrations of Venusian creatures appeared in many popular magazines of the day. No life, however, has ever been found on the planet. Because of the atmosphere, direct photography of Venus' surface is impossible. The only method of exploring the planet from Earth is by using radar. In recent years, the US and former USSR have sent many missions to explore Venus, including:-The Mariner missions, begun in December 1962 by the US.-The Venera missions, begun in February 1966 by the USSR.-The Pioneer missions, begun in 1978 by the US.-The Magellan missions, begun in 1989 by the US.</text>
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<text>MarsPlanet statisticsDistance from the Sun: Maximum:154.5 million miles 249.1 million km 1.667 AU Minimum:128.5 million miles 206.7 million km 1.381 AU Mean: 141.5 million miles 227.9 million km 1.524 AUPeriod of revolution: 687.0 daysPeriod of rotation (equatorial): 24 hr. 37 min. 23 sec.Mean orbital velocity: 15 miles (24.1 km) per secondInclination of axis: 23.98 degreesOrbital eccentricity: 0.093Orbital inclination: 1.85 degreesDiameter at equator: 4,222 miles (6,794 km) 0.547 x EarthΓÇÖs diameterOblateness: 0.006Mass: 6.42 x 10^23 kg 0.107 x EarthΓÇÖs massVolume: 1.63 x 10^11 km^3 0.15 x EarthΓÇÖs volumeDensity: 3.94 g/cm^3 0.712 x EarthΓÇÖs densitySurface gravity: 3.72 m/s^2 0.38 x EarthΓÇÖs gravityEscape velocity: 3.2 miles (5.0 km) per secondMean surface temperature: -9 F / -23 C / 250 KMaximum apparent diameter as seen from Earth (seconds of arc): 25.7ΓÇ¥Albedo: 0.16Number of known satellites: 2Mean diameter of Sun as seen from the planet: 21' 00"Satellite dataPhobosMean distance from center of Mars: 5,830 mi. (9,380 km)Inclination of Axis: 0 degreesRotation period: 0.319 daysOrbital period: 0.319 daysOrbital eccentricity: 0.018Orbital inclination to Mars' equator: 1.1 degreesDiameter: 17 x 14 x 11 mi. (27 x 22 x 18 km)Mass: 9.6 x 10^15 kgDensity: 1.9 g/cm^3Escape velocity: 0.01 miles (0.016 km) per secondMaximum apparent diameter as seen from Mars: 12' 3"DeimosMean distance from center of Mars: 14,600 mi. (23,500 km)Inclination of Axis: 0 degreesRotation period: 1.262 daysOrbital period: 1.262 daysOrbital eccentricity: 0.003Orbital inclination to Mars' equator: 2.8 degreesDiameter: 6 x 7 x 9 mi. (10 x 12 x 15 km)Mass: 2.0 x 10^15 kgDensity: 2.1 g/cm^3Escape velocity: 0.005 miles (0.008 km) per secondMaximum apparent diameter as seen from Mars: 1' 7"Planet compositionResearchers are not certain whether Mars has a core, but they speculate that it would be iron-rich and smaller than Earth's. Surrounding the core is a thick mantle, composed of silicates. The thin crust is covered by reddish oxides, which give the planet its color. Rocks on the surface are volcanic in origin and are composed mainly of iron (18%) and silicon (45%). Traces of magnesium, sulphur, and aluminum are also present.The youngest surface on Mars lies at the poles, which are covered with white ice caps that wax and wane with the seasons. The northern pole is covered with water ice, while the southern pole has dry, carbon dioxide ice.Mars is smaller and less dense than Earth. In fact, Mars has the lowest density of all the terrestrial planets (3.9). Its diameter (6,749 km) is half the Earth's and twice the Moon's.Core: radius of 1500 to 2000 kmMantle: 1300 to 1800 km thickCrust: 25 to 40 km thickTopographyEvidence suggests that the planet had a denser atmosphere in the past that allowed water to flow on the planet. Physical features closely resembling shorelines, gorges, riverbeds, and islands suggest that great rivers once marked the planet.The surface of Mars is covered with craters resulting from volcanic activity and impact. The southern hemisphere of the globe is more densely cratered than north. The two largest craters in south are Hellas (1,800 km in diameter) and Argyre (800 km). Helles is the deepest on Mars, lying 3 km below the planet surface.The northern hemisphere hosts several gigantic shield volcanoes that rise from the broad Tharsis "bulge" and from a smaller raised area in Elysium to the west. Extending eastward from Tharsis is an immense canyon system├│Valles Marineris. The largest surface feature on the planet, Valles Marinaris stretches over 3,000 miles and reaches widths up to 450 miles. Radiating outward are arrays of tension faults (graben). Valles Marineris ends in an huge region of chaotic terrain between Chryse Planitia and Margaritifer Sinus. North of the canyons are outflow channels that appear to be the result of catastrophic flooding between 3,500 and 3,000 million years ago. Mars has the largest volcanoes known in the solar system. Olympus Mons, the largest on Mars , is 25 km high and has a volume between 50 and 100 times that of Mauna Loa, the largest volcano on Earth. At its summit lies an enormous caldera at least 80 km in diameter.AtmosphereLike Earth, the Martian atmosphere is composed of gases released from the interior through volcanic activity. Mars' atmosphere is 95% carbon dioxide, 2% nitrogen, and 1.6% argon. In addition, traces of water vapor, carbon monoxide, oxygen, ozone, krypton, neon, and xenon are present. Unlike Earth, the Mars has no ozone layer, which means the planetΓÇÖs surface is fully exposed to ultraviolet radiation.The atmosphere of Mars is tenuous; the surface pressure is less than 1% of the EarthΓÇÖs. Since the atmosphere is so thin, it cannot scatter shorter-wavelength radiation from the Sun (the phenomenon that makes the Earth's sky blue). As a result, the Martian sky is pink. Because of the tilt of its axis, Mars also exhibits a seasonal pattern similar to Earth, although it is much colder.Temperatures at the equator range from a summer high of approximately 4F / -20C / 253 K in the afternoon to -168 F / -111 C / 162 K just before sunrise. The large range in temperature contributes to causing frequent dust storms, which sometimes engulf the entire planet.Magnetic field and gravityMars has only a slight magnetic field. Though the field is stronger than Venus', Mars' ionosphere and bow shock are much weaker because of its sparse atmosphere.The surface gravity on the planet is 0.38 times the EarthΓÇÖs gravity.Orbit and rotationCompared with Earth, Mars has an eccentric orbit. Its period of revolution is 687 days.Moons (and/or rings)Mars has two satellites: Phobos and Deimos. Both were discovered by Asaph Hall in 1877. Researchers believe that the moons were originally asteroids that ventured too close to Mars and were captured by its gravity.Phobos is heavily cratered. The largest is crater, Stickney, is 10 km in diameter. Deimos is relatively smooth in comparison. It has no craters larger than 3 km) The two most prominent craters are named Swift and Voltair. Both satellites are covered with a thin layer of dust. MythologyIts blood-like color earned the planet the name Mars, for the Roman god of War. It's satellites, Phobos (fear) and Deimos (terror), were named after mythical characters who drove the chariot of Mars. Discovery and explorationOf all the planets, Mars has long been considered the solar system's prime candidate for harboring extraterrestrial life. Astronomers studying the red planet through telescopes saw what appeared to be straight lines cross-crossing the surface. These observations (later determined to be optical illusions) led to the popular notion that intelligent beings had constructed a system of irrigation canals on the planet. This belief was further propagated by the writings of Jules Verne in the late 1800's and by early 20th-century movies. Another reason for scientists to expect life on Mars had to do with the apparent seasonal color changes on the planet surface. This phenomenon led to speculation that conditions might support bloom of Martian vegetation during the warmer months and cause plant life to become dormant during cooler periods.The planet has been heavily researched in modern times. In 1965, the Mariner 4 probe passed Mars at 10,000 km. Mariner 6 and 7 passed by in 1969, and Mariner 9 orbited the planet from October 1971 - 1972. Based on photos returned by Mariner 9, researchers were able to create first reliable map of the Martian surface. In September 1975, NASA launched two Viking probes launched with the goal of landing one on each hemisphere of Mars. The landers reached Mars in June and August 1976 and both landings were successful. Initial test results on samples taken from surface seemed to indicate biological activity, but later tests confirmed that the activity was inorganic. Despite the inconclusive results of the Viking biology experiments, we know more about Mars than any other planet except Earth.</text>
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<text><span class="style2">ercuryPlanet statisticsDistance from the Sun: Maximum: 43.3 million miles 69.7 million km 0.467 AU Minimum: 28.5 million miles 45.9 million km 0.306 AUMean: 36 million miles 57.9 million km 0.387 AUPeriod of revolution: 87.97 daysPeriod of rotation (equatorial): 58.65 daysMean orbital velocity: 29.7 miles (47.9 km) per secondInclination of axis: 0 degreesOrbital eccentricity: 0.206Orbital inclination: 7.0 degreesDiameter at equator: 3,033 miles (4,879 km) 0.382 x Earth's diameterOblateness: 0Mass: 3.30 x 10^23 kg 0.055 x EarthΓÇÖs massVolume: 6.07 x 10^10 km^3 0.056 x EarthΓÇÖs volumeDensity: 5.43 g/cm^3 0.984 x EarthΓÇÖs densitySurface gravity: 2.78 m/s^2 0.38 x EarthΓÇÖs gravityEscape velocity: 2.6 miles (4.3 km) per secondMean surface temperature: 662 F / 350 C / 623 K (day) -274 F / -170 C / 103 K (night)Maximum apparent diameter as seen from Earth (seconds of arc): 12".9Albedo: 0.1Number of known satellites: 0Mean diameter of Sun as seen from the planet: 1 22' 40"Planet compositionMercuryΓÇÖs radius is 2440 km and its density is 5.43 g/cm^3. These two facts, in addition to information about its magnetic field, lead scientists to believe that Mercury has a relatively large iron core composed of 65 to 75% iron. Surrounding the core is a mantle probably composed of iron and magnesium silicates and a crust thought to be composed of calcium, sodium, and other silicates. However, it is possible that Mercury does not have a chemically distinct crust. If the hypothesis about the sizes and compositions of the core and mantle are correct, Mercury is apporoximately twice as rich in iron as any other planet in the solar system.Core: radius of 1800 kmMantle: 460 km thickCrust: 180 km thickAtmosphereThe planet has only a trace atmosphere, composed mainly of argon, neon, and helium, and its surface pressure is one trillionth of the pressure on Earth. Mercury boasts the largest surface temperature variance in the solar system, ranging from -298 F / -183 C / 90 K on the night side to 872 F / 467 C / 740 K on the day side.Magnetic fields and gravityMercury possesses a magnetic field, but its strength is only one-hundredth the strength of the Earth's. Possible explanations for the magnetic field include a dynamo in Mercury's large iron core, a "fossil" field which once existed and magnetized the iron and rocks, and an induced field caused by iteractions with the Sun. However, none of these theories completely explains the measured field. The magnetic field causes a magnetosphere similar to the Earth's but without radiation belts.The surface gravity on Mercury is 0.38 times the surface gravity on Earth..Orbit and rotationObit has a mean radius of only 36 million miles (58 million km), which means it's usually too close to the sun to be seen. Mercury spins only three times on its axis in the course of two of its years.With the exception of Pluto, Mercury has the most eccentric orbit of all the planets. TopographyMercury is difficult to observe from Earth because it's never seen against a dark background (the best observation times being near sunrise and sunset, when the same feature are always pointed toward Earth). Most of our knowledge of Mercury is a result of the 1974 Mariner 10 flyby.Craters are the main topographical feature on the planet. Most were created approximately 4 to 4.5 million years ago and range from 100m to 1,000 km in diameter. Mercury also has plains, which researchers believe were formed later in Mercury's evolution. Other features include scarps and troughs, which are probably the result of tectonic activity.The planet's northwest quadrant is dominated by the Caloris Basin (1,300 km in diameter), the largest structural feature on Mercury. The northeast quadrant contains a smooth plain (Borealis Planitia) and a large lava-flooded basin, 310 km in diameter. There are also several prominent ray craters, including Rodin; a double ring basin surrounded by other major craters. The southwest quadrant consists mainly of inter-crater plains. The largest crater in the region is Beethoven (625 km wide; the second-largest known crater on Mercury). The southeast quadrant is the most heavily cratered and probably the oldest. This region also hosts three relatively young ray craters (Coply, Snorri, and Kuiper) and eight of 16 named scarps on the planet.Moons and/or ringsThere are no known moons or rings associated with Mercury.MythologyThis planet was known to the Egyptians and Greeks, who named it after Hermes (Mercury), the messenger of the Gods and deity of science, eloquence, and cunning. In ancient astrology, a child born under Mercury loved learning, travel, and art. Wednesday was dedicated to Mercury, which was known to influence the kidneys of the human body.Discovery and explorationThe first Mercurian observer is believed to be Johannes Hevelius in the 17th century. First maps of Mercury were created in Milan by G. V. Schiaparelli beginning in 1821. The only exploratory probe to visit Mercury was Mariner 10. Its flyby in March 1974 provided most of what we know about Mercury today.</span></text>
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<text>Earth statisticsDistance from the Sun: Maximum: 94.2 million miles 152.1 million km 1.017 AU Minimum: 91.4 million miles 147.1 million km 0.983 AUMean: 93.0 miles 149.6 million km 1.000 AUPeriod of revolution: 365.26 daysPeriod of rotation (equatorial): 23 hr. 56 min. 4 sec.Mean orbital velocity: 18.5 miles (29.8 km) per secondInclination of axis: 23.44 degreesOrbital eccentricity: 0.017Orbital inclination: 0 degreesDiameter at equator: 7,928 miles (12,756 km)Oblateness: 0.003Mass: 5.97 x 10^24 kgVolume: 1.084 x 10^12 km^3Density: 5.52 g/cm^3Surface gravity: 9.78 m/s^2 Escape velocity: 6.94 miles (11.2 km) per secondMean surface temperature: 72F / 22 C / 295 KAlbedo: 0.39Number of known satellites: 1Mean diameter of Sun as seen from the planet: 32' 01"Satellite statisticsMoonMean distance from center of planet: 238,900 miles (384,400 km)Inclination of Axis: 6.7 degreesRotation period: 27.321 daysOrbital period: 27.321 daysOrbital eccentricity: 0.055Orbital inclination to planet's equator: 18.3 degrees to 28.6 degreesDiameter: 2,160.1 miles (3,475.6 km)Mass: 7.35 x 10^22 kgDensity: 3.34 g/cm^3Escape velocity: 1.48 miles (2.38 km) per secondMaximum apparent diameter as seen from the planet: 31' 5"Planet compositionThe core of the Earth, composed of metallic nickel iron and iron oxides, is about 6800 km (4230 miles) in diameter. The outer 2100 km of the core is molten, and the rest is solid, with a specific gravity of about 16. Surrounding the core is a mantle composed of magnesium and iron silicates. On top of thte mantle is a thin crust, approximately 33 km thick, which is divided into 15 plates. The composition of the crust varies: under the continents it consists of a substrata of granite rock, rich in silicon and aluminum, and under the oceans it is primarily basalt rocks, rich in silicon and magnesium.Inner core: radius of 1300 kmLiquid outer core: 2100 km thickMantle: 2945 km thickCrust: 33 km thickTopographyThe Earth is unlike the other terrestrial planets. Aside from being host to the only known life forms in the solar system, Earth has very few craters, many volcanic plains, and 70% of the surface is covered by water. Our planet also has folded mountain chains and platform deposits, which occur nowhere else in our solar system.Erosion, weather, sea-floor spreading, and subduction are continually changing the outer face of the planet. The highest point on the Earth's surface is the summit of Mount Everest (29,028 ft.). The largest feature on the face of the planet is the Pacific Ocean (64,186,000 sq. mi. or 166,883,600 sq. km).AtmosphereThe Earth's atmosphere today is thought to be the result of volcanic activity and the presence of living organisms, which produce oxygen through photosynthesis. Between sea level and an altitude of about 10 km lies the troposphere, which consists mainly of nitrogen (78%) and oxygen (21%), with traces of water vapor, argon, and carbon dioxide. This region contains 80% of the Earth's atmosphere (by mass) and is where virtually all recognizable weather takes place. Above the troposphere lies the stratosphere, where a layer of ozone absorbs ultraviolet radiation from the Sun. In the thermosphere, which begins about 80 km from the surface, the molecules are heated by radiation from the Sun, and the temperature increases with increasing altitude. Particles that are hot enough escape from the outermost layer, the exosphere, into interplanetary space.The mean temperature on Earth is 60.53 F / 33.5 C / 306.5 K. Temperature extremes have been measured at el Azizia, Libya (136.4 F/ 75.6 C / 348.6 K) and Vostok, Antarctica (-126.9 F / -70.7 C / 202 K ).Besides affecting weather and the shape of our atmosphere, solar activity gives rise to a dramatic visual phenomenon in our atmosphere. When charged particles from the solar wind become trapped in Earth's magnetic field, they collide with air molecules above the magnetic poles and begin to glow. These glowing molecules are known as the auroras, or the northern and southern lights.Magnetic fields and gravityThe interaction of the Earth's magnetic field with the solar wind creates a bow shock and magnetosphere. The magnetic field of the Earth and other planets is similar to a dipole field--the type of field created by bar magnets. Due to the pressure of the solar wind, the magnetic field is compressed on the side of Earth facing the Sun. The magnetotail, on the other side of the Earth, streams outward for many thousands of kilometers. Within the magnetosphere are regions of charged particles which are trapped by the Earth's magnetic field. These regions are known as the Van Allen radiation belts. Earth is the densest planet in the solar system, having a density of 5.52 g/cm^3 (water has a density of 1 g/cm^3). The surface gravity is 9.78 m/s^2.Orbit and rotationThe Earth has an elliptical orbit with an eccentricity of 0.0167. Its orbital speed is 29.79 km/s.Moons and/or ringsEarth has one satellite: The Moon. From rocks and materials gathered on the Apollo expeditions, researchers have been able to conclude the Moon is between 4.0 and 4.3 billion years old. Its origins are a mystery. Four theories attempt an explanation: The moon formed near Earth as a separate body; it was torn from Earth; it formed somewhere else and was captured by our planet's gravity, or it was the result of a collision between Earth and an asteroid about the size of Mars. The first few million years of the Moon's existence were so violent that few traces of this period remain. As a molten outer layer gradually cooled and solidified into different layers of rock, the Moon was bombarded by huge asteroids and smaller objects. Some of the asteroids were as large as Rhode Island or Delaware and their collisions with the Moon created basins hundreds of kilometers across. The bombardment tapered off approximately four billion years ago, leaving the lunar highlands covered with huge, overlapping craters and a deep layer of shattered and broken rock. Heat produced by the decay of radioactive elements began to melt the interior of the Moon at depths of about 200 km (125 miles) below the surface. Then, for the next 700 million years (from about 3.8 to 3.1 billion years ago) lava rose from inside the Moon and gradually spread out over the surface, flooding the large impact basins to form the dark areas that Galileo Galilei called maria (meaning seas). As far as researchers can tell, there has been no significant volcanic activity on the Moon since then. The surface of the planet has been altered by atomic particles from the sun and stars, by the rare impacts of large meteorites, and by spacecraft and astronauts.MythologyFor many ages, the Earth was considered the center of the universe. It was also considered to be a flat disk or a square plate floating on the oceans. The Earth and atmosphere were composed of four elements: water, air, earth, and fire. Some believed in a fifth element: ether or space. The sky was believed to be a shell formed of solid crystalline material, studded with lights, and resting at the edges of the Earth. It was also believed that our world was sustained by animals, folk heroes, and other means. For example, Greeks placed the world on the shoulders of Atlas, the Vedic priests placed it on in pillars, the Hindus on the backs of animals, and the Norsemen in the branches of the world tree.Discovery and explorationFirst American satellite├│Explorer 1├│was launched from Cape Canaveral in Florida on Jan. 31, 1958 and brought to researchers' attention the intense radiation zone surrounding Earth, known as the Van Allen Belts. Between 1964 and 1968, the automated Ranger, Surveyor, and Lunar Orbiter spacecraft were dispatched by NASA to study the Moon . The first human footsteps on another planet were made by the Apollo expedition crews from 1969 to 1972.</text>
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<text>Saturn statisticsDistance from the Sun: Maximum: 934.3 million miles 1,507 million km 10.069 AU Minimum: 835.1 million miles 1,347 million km 9.009 AU Mean: 884.7 million miles 1,427 million km 9.539 AUPeriod of revolution: 29.46 yearsPeriod of rotation (equatorial): 10 hr. 14 min.Mean orbital velocity: 6 miles (9.6 km) per secondInclination of axis: 26.73 degreesOrbital eccentricity: 0.056Orbital inclination: 2.49 degreesDiameter at equator: 74,990 miles (120,660 km) 9.41 x EarthΓÇÖs diameterOblateness: 0.102Mass: 5.69 x 10^26 kg 95.1 x EarthΓÇÖs massVolume: 8.15 x 10^14 km^3 752 x EarthΓÇÖs volumeDensity: 0.69 g/cm^3 0.127 x EarthΓÇÖs densitySurface gravity: 11.3 m/s^2 1.16 x EarthΓÇÖs gravityEscape velocity: 22.1 miles (35.6 km) per secondMean surface temperature: -292 F / -180 C / 93 K (at cloud tops)Maximum apparent diameter as seen from Earth: 20.9"Albedo: 0.46Number of known satelites: 18Mean diameter of Sun as seen from Saturn: 3' 22"Planet compositionWith a density only 0.69 times that of water, Saturn is the least dense of all the planets. (Terrestrial planets like Earth , Mercury, Venus, and Mars have densities closer to 5 times that of water.) Saturn's mass, however, is 95 times greater than Earth and is second only to Jupiter.Like Jupiter, Saturn is believed to have a relatively small, rocky core, although Saturn may also have a layer of water, methane, and ammonia ices surrounding its core. Two thick layers of liquid hydrogen surround the central regions. In the lower layer, the pressure is so great that hydrogen behaves like a metal. As is the case with Jupiter, it is thought that the motion and circulation of this metallic layer give rise to Saturn's magnetic field. A gaseous atmosphere of hydrogen and helium lies above the upper layer of liquid hydrogen. Rocky Core: radius of 13000 kmLiquid Helium Layer: 2000 km thickLiquid Metallic Hydrogen Layer: 26000 km thickLiquid Hydrogen Layer: 18000 km thickHydrogen and Helium Gas Layer: 1500 km thickTopographyA wide range of cloud systems exist in Saturn' atmosphere. Several persistent symmetric white, brown, and red ovals have been observed at various latitudes and are believed to be a product of mixing methane, ammonia, and sulfur. Atmospheric bands colored yellow, brown, and black are the result of molecules, which were destroyed by ultraviolet sunlight and violent lightening, being mixed together by Saturn's dynamic weather patterns. The red band is probably produced by phosphine. Two main atmospheric belts North Equatorial (Latitude +20) and South Equatorial (Latitude -20) are always visible, and aurora are common between 78 and 80 Latitude in both hemispheres. The major cloud features in Saturn's northern hemisphere are the Brown spot (1, 5,00 km in diameter) and Big Bertha (the largest spot, measuring 10,000 by 6,000 km). Saturn's southern hemisphere features Anne's Spot (5,000 by 3,000 km).Compared with Jupiter, Saturn's features are low-contrast. This is explained in part by Saturn's lower temperatures and weaker gravity. The lower temperature means that the condensation point for a compound such as ammonia is reached at higher pressure (lower altitude or greater atmospheric depth) on Saturn.AtmosphereHydrogen is the most abundant element in Saturn's atmosphere (about 94% by volume), followed by helium (about 6%). Traces of ammonia, phosphine, methane, ethane, acetylene, ammonium hydrosulfide, and water vapor are also present. A wide range of cloud systems exist in Saturn's atmosphere, with clouds of different compositions typically occurring in different layers (as seen in the diagram to the left). The winds at Saturn's equator have been measured at 1,770 km (1,100 miles) per hour. These powerful winds, as well as other dynamic weather patterns, mix different molecules together to produce atmospheric bands colored yellow, brown, and black. Saturn's atmospheric features are not as colorful as those of Jupiter, probably because different chemical reactions predominate at Saturn's cooler temperatures. Despite the 27 inclination of the axis of rotation, Saturn's winds are symmetrical with respect to the equator. This indicates that the weak radiation received from the Sun only slightly affects atmospheric motion.Magnetic fields and gravityLike other planetary magnetic fields, the magnetic field generated by the liquid metallic hydrogen in Saturn's interior is very similar to that created by a simple bar magnet with north and south poles. Unlike other planets, however, Saturn's magnetic axis is aligned to within 1 degree of the spin axis.The bow shock is approximately 24 Saturn radii away from the planet on the side closest to the Sun. On the opposite side of the planet, the magnetic field becomes very stretched and forms the magneto tail. The magneto tail extends for hundreds of radii away from Saturn; at a distance of 25 Saturn radii, the diameter of the tail is 80 Saturn radii.Titan has no intrinsic magnetic field; therefore it has no electrically conducting and convecting liquid core. Its interaction with Saturn's magnetosphere creates a magnetic wake behind Titan. The big satellite also serves as a source for both neutral and charged hydrogen atoms in Saturn's magnetosphere.Surface gravity on Saturn is 1.19 times the gravity on Earth.Orbit and rotationSaturn orbits in a very eccentric pattern at a mean distance of 1,427 million km from the Sun. It has a very rapid axial rotation of 10 hours 15 minutes, and an orbital period of 10,759.2 days (29.46 Earth years).Moons and/or ringsSaturn has more than 20 known satellites, more than any other planet in the solar system. All of Saturn's satellites contain a high percentage of ice, but each is unique: Dione is dense; Mimas is marked by a crater 1/3 the size of the satellite; Enceladus has a smooth surface; Hyperion has an irregular shape; and Phoebe has a retrograde rotation. The largest satellite, Titan, has a dense, nitrogen-based atmosphere that makes it unique among all the solar system satellites. Researchers believe that solar radiation may be converting methane in Titan's atmosphere to ethane, acetylene, and (in combination with nitrogen) hydrogen cyanide, the building block of amino acids. These conditions may be similar to the conditions present on Earth between three and four billion years ago, but scientists believe that Titan's temperature is too low to permit further organic evolution.Saturn is also surrounded by a series of seven named major rings (" A" through "G"), which have variable compositions. Researchers speculate that the rings were formed when a large object encountered Saturn early on in the solar system's evolution and broke into tiny fragments that spread around the planet. Alternatively, it is possible that a single, large satellite orbiting Saturn was destroyed by a collision with another object such as an asteroid. There is growing support for the theory that the rings represent debris associated with Saturn as the planet evolved from the original solar nebula, and that the debris was never part of another body. The main rings A, B, and probably contain water ice in pieces ranging from tiny grains to blocks several tens of meters in diameter. Together the main rings span a width of about 275,000 km. Rings A and B are divided by the Cassini Division, a gap as wide as North America (nearly 4,000 km). Ring C, known as the Crepe or Dusky Ring, is semi-transparent. Some of the known rings were not discovered by land-based observers. Pioneer 11 first detected Ring F and the Voyager probes added G and E, which are both very tenuous. The Voyagers also provided proof that there are literally thousands of rings within the minor divisions in major rings.MythologyNamed for Cronos, father of Zeus (Jupiter). Most satellites are named for Titans who, according to Greek mythology, were brothers and sisters of Saturn. Janus is named for the two-faced Roman god who could look forward and backward at the same time. Epimetheus was named for the backward looking god. Mimas for a titan felled by Hephaestus (or Ares) in the war between the titans and Olympian gods. In that same war, Enceladus was crushed by Athene and earth piled on top of him became the island of Sicily. Tethys was the wife of Oceanus and mother of all rivers and Oceanids. Dione was the sister of Cronos and mother (by Zeus) of Aphrodite. Rhea, another sister of Cronos, was also his wife. Hyperion and Iapetus were also titans.Discovery and explorationSaturn, named for Jupiter's father, the first ruler of Olympus, is the most remote planet known to ancient people. The first recorded observations were made in Mesopotamia in the mid-7th century BC when Saturn occulted the Moon. Galileo Galilei is credited with the first observations of the disk itself in 1610. And in 1659, the rings were accurately described for the first time by Christiaan Huygens. G.D. Cassini, director of the Paris Observatory, first noted the gap in the rings in 1675, now known as Cassini's Division. The cause for the division was first explained by the "zones of avoidance" theory (the same as theory used to describe the reason for gaps between minor planets and asteroids between the Sun and Mars and Jupiter), developed in 1866 by Daniel Kirkwood.In modern times, Saturn has been visited by Pioneer and Voyager probes: Pioneer 11 visited in September 1979. Voyager 1 in November 1980; Voyager 2 in August 1981. Exploration of the planet will continue with the Cassini mission, a combined effort by NASA and the European Space Agency scheduled for launch the latter part of the 1990s.Satellite dataPan (S18)Mean distance from center of Saturn: 83,000 miles (133,600 km)Inclination of axis: unknownRotation period: unknownOrbital period: 0.576 daysOrbital eccentricity: 0Orbital inclination to Saturn's equator: 0 degreesDiameter: 12 miles (20 km)Mass: unknownDensity: unknownEscape Velocity: 0.006 mile (0.01 km) per secondMaximum apparent diameter as seen from Saturn: unknownAtlas (S15)Mean distance from center of Saturn: 85,560 miles (137,670 km)Inclination of axis: unknownRotation period: unknownOrbital period: 0.602 daysOrbital eccentricity: 0.002Orbital inclination to Saturn's equator: 0.3 degreesDiameter: 23 x 21 x 27 miles (37 x 34 x 27 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.009 mile (0.015 km) per secondMaximum apparent diameter as seen from Saturn: unknownPrometheus (S16)Mean distance from center of Saturn: 86,600 miles (139,350 km)Inclination of axis: unknownRotation period: unknownOrbital period: 0.613 daysOrbital eccentricity: 0.004Orbital inclination to Saturn's equator: 0.0 degreesDiameter: 92 x 62 x 42 miles (148 x 100 x 68 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.03 mile (0.05 km) per secondMaximum apparent diameter as seen from Saturn: unknownPandora (S17)Mean distance from center of Saturn: 88,100 miles (141,700 km)Inclination of axis: unknownRotation period: unknownOrbital period: 0.629 daysOrbital eccentricity: 0.004Orbital inclination to Saturn's equator: 0.05 degreesDiameter: 68 x 55 x 39 mi. (110 x 88 x 62 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mi (0.035 km) per secondMaximum apparent diameter as seen from Saturn: unknownEpimetheus (S11)Mean distance from center of Saturn: 94,110 miles (151,420 km)Inclination of Axis: unknownRotation period: unknownOrbital period: 0.694Orbital eccentricity: 0.009Orbital inclination to Saturn's equator: 0.34 degreesDiameter: 86 x 68 x 68 miles (138 x 110 x 110 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.03 mile (0.45 km) per secondMaximum apparent diameter as seen from Saturn: unknownJanus (S10)Mean distance from center of Saturn: 94,140 miles (151,470 km)Inclination of axis: unknownRotation period: unknownOrbital period: 0.695 daysOrbital eccentricity: 0.007Orbital inclination to Saturn's equator: 0.14 degreesDiameter: 118 x 121 x 96 miles (190 x 194 x 154 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.045 mi (0.075 km) per secondMaximum apparent diameter as seen from Saturn: unknownMimas (S1)Mean distance from center of Saturn: 115,300 miles (185,540 km)Inclination of axis: 0 degreesRotation period: 0.942 daysOrbital period: 0.942 daysOrbital eccentricity: 0.020Orbital inclination to planet's equator: 1.52 degreesDiameter: 247 miles (398 km)Mass: 4.5 x 10^19 kgDensity: 1.2 g/cm^3Escape velocity: 0.10 mi (0.16 km) per secondMaximum apparent diameter as seen from Saturn: 10' 54"Enceladus (S2)Mean distance from center of Saturn: 147,940 miles (238,040 km)Inclination of axis: 0 degreesRotation period: 1.370 daysOrbital period: 1.370 daysOrbital eccentricity: 0.004Orbital inclination to Saturn's equator: 0.02 degreesDiameter: 310 miles (498 km)Mass: 8.4 x 10^19 kgDensity: 1.2 g/cm^3Escape velocity: 0.12 mile (0.2 km) per secondMaximum apparent diameter as seen from Saturn: 10' 36"Tethys (S3)Mean distance from center of Saturn: 183,140 miles (294,670 km)Inclination of axis: 0 degreesRotation period: 1.888 daysOrbital period: 1.888 daysOrbital eccentricity: 0.0Orbital inclination to Saturn's equator: 1.1 degreesDiameter: 650 miles (1,046 km)Mass: 7.5 x 10^20 kgDensity: 1.21 g/cm^3Escape velocity: 0.25 mile (0.4 km) per secondMaximum apparent diameter as seen from Saturn: 17' 36"Telesto (S14)Mean distance from center of Saturn: 183,140 miles (294,670 km) (Leads Tethys by 60 degrees)Inclination of axis: unknownRotation period: unknownOrbital period: 1.888 daysOrbital eccentricity: 0.0Orbital inclination to Saturn's equator: 1 degreeDiameter: 19 x 16 x 10 miles (30 x 26 x 16 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.006 mile (0.01 km) per secondMaximum apparent diameter as seen from Saturn: unknownCalypso (S13)Mean distance from center of Saturn: 183,140 miles (294,670 km) (Trails Tethys by 60 degrees)Inclination of axis: unknownRotation period: unknownOrbital period: 1.888 daysOrbital eccentricity: 0Orbital inclination to Saturn's equator: 1 degreeDiameter:19 x 10 x 10 miles (30 x 16 x 16 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.006 mi (0.01 km) per secondMaximum apparent diameter as seen from Saturn: unknownDione (S4)Mean distance from center of Saturn: 234,570 miles (377,420 km)Inclination of axis: 0 degreesRotation period: 2.737 daysOrbital period: 2.737 daysOrbital eccentricity: 0.002Orbital inclination to Saturn's equator: 0.02 degeesDiameter: 696 miles (1,120 km)Mass: 1.05 x 10^21 kgDensity: 1.43 g/cm^3Escape velocity: 0.3 mile (0.5 km) per secondMaximum apparent diameter as seen from Saturn: 12' 24"Helene (S12)Mean distance from center of Saturn: 234,570 miles (377,420 km)Inclination of axis: unknownRotation period: unknownOrbital period: 2.737Orbital eccentricity: 0.005Orbital inclination to Saturn's equator: 0.15 degreesDiameter: 22 x 21 x 17 miles (36 x 34 x 28 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.006 mi (0.01 km) per secondMaximum apparent diameter as seen from Saturn: unknownRhea (S5)Mean distance from center of Saturn: 237,560 miles (527,040 km)Inclination of axis: 0 degreesRotation period: 4.518 daysOrbital period: 4.518 daysOrbital eccentricity: 0.001Orbital inclination to Saturn's equator: 0.35 degreesDiameter: 950 miles (1,528 km)Mass: 2.49 x 10^21 kgDensity: 1.33 g/cm^3Escape velocity: 0.37 mile (0.6 km) per secondMaximum apparent diameter as seen from Saturn: 10' 42"Titan (S6)Mean distance from center of Saturn: 759,390 miles (1,221,860 km)Inclination of axis: 0 degreesRotation period: probably 15.945 daysOrbital period: 15.945 daysOrbital eccentricity: 0.029Orbital inclination to Saturn's equator: 0.33 degreesDiameter: 3,201 miles (5,150 km)Mass: 1.35 x 10^23 kgDensity: 1.88 g/cm^3Escape velocity: 1.6 miles (2.2 km) per secondMaximum apparent diameter as seen from Saturn: 17' 10"Hyperion (S7)Mean distance from center of Saturn: 920,510 miles (1,481,100 km)Inclination of axis: unknownRotation period: unknownOrbital period: 21.277 daysOrbital eccentricity: 0.104Orbital inclination to Saturn's equator: 0.43 degreesDiameter: 224 x 174 x 140 miles (360 x 280 x 226 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.12 mile (0.2 km) per secondMaximum apparent diameter as seen from Saturn: 43"Iapetus (S8)Mean distance from center of Saturn: 2,213,360 miles (3,561,300 km)Inclination of axis: 0 degreesRotation period: 79.331 daysOrbital period: 79.331 daysOrbital eccentricity: 0.028Orbital inclination to Saturn's equator: 14.7 degreesDiameter: 892 miles (1,436 km)Mass: 1.88 x 10^21 kgDensity: 1.16 g/cm^3Escape velocity: 0.44 mile (0.7 km) per secondMaximum apparent diameter as seen from Saturn: 1' 48"Phoebe (S9)Mean distance from center of Saturn: 8,051,000 miles (12,954,000 km)Inclination of axis: unknownRotation period: approx. 0.4 daysOrbital period: 550.4 daysOrbital eccentricity: 0.163Orbital inclination to Saturn's equator: 150 degreesDiameter: 137 miles (220 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.06 mile (0.1 km) per secondMaximum apparent diameter as seen from Saturn: 3"</text>
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<text>Uranus statisticsDistance from the SunMaximum: 1,867 million miles 3,004 million km 20.088 AUMinimum: 1,699 million miles 2,735 million km 18.275 AUMean: 1,783 million miles 2,870 million km 19.82 AUPeriod of revolution: 84.01 yearsPeriod of rotation (equatorial): 17 hr. 14 min.Mean orbital velocity: 4.2 miles (6.8 km) per secondInclination of axis: 97.9 Orbital eccentricity: 0.047Orbital inclination: 0.774 Diameter at equator: 31,770 miles (51,118 km) 4.01 x Earth's diameterOblateness: 0.023Mass: 8.66 x 10^25 kg 14.6 x Earth's massVolume: 7.26 x 10^13 km^3 67 x Earth's volumeDensity: 1.17 g/cm^3 0.23 x Earth's densitySurface gravity: 11.44 m/s^2 1.17 x Earth's gravityEscape velocity: 13.2 miles (21.3 km) per secondMean surface temperature: -353 F / -214 C / 59 K (at cloud tops)Maximum apparent diameter as seen from Earth (seconds of arc): 3.7"Number of known satellites: 15Mean diameter of Sun as seen from the planet: 1' 41"Satellite dataCordelia (U6)Mean distance from center of Uranus: 30,746 miles (49,471 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.335 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.14 Diameter: 16 miles (26 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.006 mile (0.01 km) per secondMaximum apparent diameter as seen from Uranus: unknownOphelia (U7)Mean distance from center of Uranus: 33,434 miles (53,796 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.372 daysOrbital eccentricity: 0.01Orbital inclination to Uranus' equator: 0.09 Diameter: 19 miles (30 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.006 mile (0.01 km) per secondMaximum apparent diameter as seen from Uranus: unknownBianca (U8)Mean distance from center of Uranus: 36,776 miles (59,173 km)Inclination of Axis: approx. 0 Rotation period: unknownOrbital period: 0.431 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.16 Diameter: 26 miles (42 km)Mass: unknownDensity: unknownEscape velocity: approx.0.01 mile (0.02 km) per secondMaximum apparent diameter as seen from Uranus: unknownCressida (U9)Mean distance from center of Uranus: 38,395 miles (61,777 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.463 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.04 Diameter: 39 miles (62 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mile (0.03 km) per secondMaximum apparent diameter as seen from Uranus: unknownDesdemona (U10)Mean distance from center of Uranus: 38,953 miles (62,676 km)Inclination of Axis: approx. 0 Rotation period: unknownOrbital period: 0.475 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.16 Diameter: 34 miles (54 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mile (0.03 km) per secondMaximum apparent diameter as seen from Uranus: unknownJuliet (U11)Mean distance from center of Uranus: 39,995 miles (64,352 km)Inclination of Axis: approx. 0 Rotation period: unknownOrbital period: 0.493 daysOrbital eccentricity: 0Orbital inclination to Uranus equator: 0.06 Diameter: 52 miles (84 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.025 mile (0.04 km) per secondMaximum apparent diameter as seen from Uranus: unknownPortia (U12)Mean distance from center of Uranus: 41,072 miles (66,085 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.513 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.09 Diameter: 67 miles (108 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.03 mile (0.05 km) per secondMaximum apparent diameter as seen from Uranus: unknownRosalind (U13)Mean distance from center of Uranus: 41,604 miles (69,941 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.558 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.28 Diameter: 34 miles (54 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mile (0.03 km) per secondMaximum apparent diameter as seen from Uranus: unknownBelinda (U14)Mean distance from center of Uranus: 46,773 miles (75,258 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.622 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.03 Diameter: 41 miles (66 km)
Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mile (0.03 km) per secondMaximum apparent diameter as seen from Uranus: unknownPuck (U15)Mean distance from center of Uranus: 53,450 miles (86,000 km)Inclination of Axis: approx. 0 Rotation period: unknownOrbital period: 0.762 daysOrbital eccentricity: 0Orbital inclination to Uranus' equator: 0.31 Diameter: 96 miles (154 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.04 mile (0.07 km) per secondMaximum apparent diameter as seen from Uranus: unknownMiranda (U5)Mean distance from center of Uranus: 80,423 miles (129,400 km)Inclination of axis: 0 Rotation period: 1.414 daysOrbital period: 1.414 daysOrbital eccentricity: 0.0Orbital inclination to Uranus' equator: 3.4 Diameter: 293 miles (472 km)Mass: 6.89 x 10^19 kgDensity: 1.35 g/cm^3Escape velocity: 0.12 mi (0.2 km) per secondMaximum apparent diameter as seen from Uranus: 17'54"Ariel (U1)Mean distance from center of Uranus: 118,710 miles (192,000 km)Inclination of axis: 0 Rotation period: 2.520 daysOrbital period: 2.520 daysOrbital eccentricity: 0.003Orbital inclination to Uranus' equator: 0.0 Diameter: 720 miles (1,158 km)Mass: 1.26 x 10^21 kgDensity: 1.66 g/cm^3Escape velocity: 0.35 mile (0.56 km) per secondMaximum apparent diameter as seen from Uranus: 30'54"Umbriel (U2)Mean distance from center of Uranus: 165,500 miles (266,300 km)Inclination of axis: 0 Rotation period: 4.144 daysOrbital period: 4.144 daysOrbital eccentricity: 0.004Orbital inclination to Uranus' equator: 0.0 Diameter: 727 miles (1,169 km)Mass: 1.33 x 10^21 kgDensity: 1.51 g/cm^3Escape velocity: 0.34 mi (0.54 km) per secondMaximum apparent diameter as seen from Uranus: 14'12"Titania (U3)Mean distance from center of Uranus: 270,300 miles (435,000 km)Inclination of axis: 0 Rotation period: 8.706 daysOrbital period: 8.706 daysOrbital eccentricity: 0.002Orbital inclination to Uranus' equator: 0.0 Diameter: 981 miles (1,578 km)Mass: 3.48 x 10^21 kgDensity: 1.68 g/cm^3Escape velocity: 0.48 mile (0.77 km) per secondMaximum apparent diameter as seen from Uranus: 15'00"Oberon (U4)Mean distance from center of Uranus: 362,600 miles (583,500 km)Inclination of axis: 0 Rotation period: 13.463 daysOrbital period: 13.463 daysOrbital eccentricity: 0.001Orbital inclination to Uranus' equator: 0.0 Diameter: 947 miles (1,523 km)Mass: 3.03 x 10^21 kgDensity: 1.58 g/cm^3Escape velocity: 0.44 mile (0.71 km) per secondMaximum apparent diameter as seen from Uranus: 9'48"Planet compositionUranus has a rocky core about the size of Earth, composed of heavy elements, mainly silicon and iron. An icy mantle of water, methane, and ammonia surrounds the core. Like Jupiter and Saturn, Uranus does not have a "surface"; above the ice a mixture of hydrogen, helium, and methane extends outward, gradually decreasing in density toward the top of the atmosphere. However, since a higher proportion of the planet is rock and ice, Uranus is more dense than its larger cousins. Rocky Core: radius of 7,000 kmIce and Water Layer: 8,000 km thickGas Layer: 10,500 km thickTopographyUranus has no distinct topographical features.AtmosphereUranus has a cold, hydrogen-rich (83% by volume) atmosphere, with a higher percentage of methane (2%) than any other planet. Most of the remainder of the atmosphere is composed of helium. Temperatures near the upper atmosphere (at the tops of the clouds) average -353 F / -214 C / 59 K and wind speeds average 580 km (360 miles) per hour. These temperatures are so cold that even methane will condense from a gas to a liquid; it is proposed that overlying the cloud layers is a layer of liquid methane. It is this layer that causes the absortion of red and near infrared light, which in turn creates the planet's blue-green appearance. The cloud layers are probably similar to those of Jupiter and Saturn, with regions of ammonia, ammounium hydrosulfide, and water ice layers. However, these layers must lie deeper in the atmosphere in order for the temperatures to be conducive to cloud formation.Magnetic fields and gravityThe intensity of the magnetic field at Uranus's surface is roughly comparable to that of Earth's, though it varies much more from point to point because of its large offset from the center of Uranus. The magnetic field source is unknown; the electrically conductive, super-pressurized ocean of water and ammonia once thought to lie between the core and the atmosphere now appears to be nonexistent. The magnetic fields of Earth and other planets are believed to arise from electrical currents produced in their molten or metallic cores.There is a magnetic tail extending millions of miles behind Uranus. Voyager measured the magnetotail to at least 10 million kilometers (6.2 million miles) behind the planet. The extreme tilt of the magnetic axis, combined with the tilt of the rotational axis, causes the field lines in this cylindrical magnetotail to be wound into a corkscrew shape.The surface gravity on Uranus is 1.17 times the gravity on Earth. Orbit and rotationThough it is not generally considered to be so, the planet's rotation is technically retrograde due to the 98 axial inclination. The orbital period is 84 years, and recent studies suggest the rotation period to be 23.9 hours. However, the lack of visible surface features makes it difficult to measure precisely. Moons and/or ringsFor many years, there were only five known satellites: Titania, Oberon, Umbrial, Ariel, and Miranda. All are half rock, half ice satellites between 520 and 1,610 km (323 - 1,000 miles) across. In 1986, Voyager 2 provided proof of the existence of 10 new moons, all between 16 - 169 km (10 - 105 miles) in diameter.The three brightest moons are Titania, Oberon, and Ariel. Their surfaces are completely covered with ice or frost, making this water the farthest from the Sun known to exist in the solar system. Miranda also features high cliffs, canyons, cratered plains, and winding valleys. Uranus also features 11 dark rings, which were discovered in 1977 when they occulted a star. They are far less reflective than Saturn's rings, and appear to be composed of dust particles less than 5k in diameter.MythologyIn Greek mythology, Uranus was the personification of the heaven and ruler of the world. He was also the father of Saturn. Miranda was named for the heroine and Ariel for the benevolent spirit in Shakespeare's play "The Tempest." Umbriel was named for the malevolent spirit in Pope's "Rape of the Lock." Titania was named for the Queen of the fairies and Oberon for the King of the fairies in Shakespeare's "Midsummer Night's Dream."Discovery and explorationUranus was discovered in 1781 by William Herschel, who also discovered the satellites Titania and Oberon (in 1787). William Lassell recovered Umbriel (previously glimpsed by Herschel) and discovered Ariel in 1851. Gerard P. Kuiper discovered Miranda in 1948. Voyager 2 did first close-up survey of Uranus in January 1986.</text>
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<text>Neptune statisticsDistance from the Sun Maximum: 2,817 million miles 4,537 million km 30.316 AU Minimum: 2,769 million miles 4,456 million km 29.800 AU Mean: 2,793 million miles 4,497 million km 30.058 AUPeriod of revolution: 164.8 yearsPeriod of rotation (equatorial): 16 hr. 3 min. or 19 hr. 12 min.Mean orbital velocity: 3.4 miles (5.4 km) per secondInclination of axis: 29.6 degreesOrbital eccentricity: 0.009Orbital inclination: 1.77 degreesDiameter at equator: 30,780 miles (49,528 km)3.96 x EarthΓÇÖs diameterOblateness: 0.017Mass: 1.02 x 10^26 kg17.2 x EarthΓÇÖs massVolume: 6.18 x 10^13 km^354 x EarthΓÇÖs volumeDensity: 1.64 g/cm^30.32 x EarthΓÇÖs densitySurface gravity: 11.0 m/s^2(Earth = 1): 1.12Escape velocity: 14.5 miles (23.3 km) per secondMean surface temperature: -364 F / -220 C / 53 K (at cloud tops)Maximum apparent diameter as seen from Earth (seconds of arc): 2.2"Albedo: 0.4Number of known satellites: 8Mean diameter of Sun as seen from the planet: 1' 04"Planet composition: The internal structure of Neptune is thought to be very much like that of Uranus. At the center of Neptune lies a core of rock and metal, with a thick layer of water, methane, and ammonia ices above it. Surrounding the ice is a layer of hydrogen, helium, and methane that reaches to the top of the atmosphere. Compared to Uranus, a larger proportion of the material in Neptune is dense rock; consequently Neptune, although its diameter is only 96% that of Uranus, is actually 18% more massive than its neighbor.Core: 8000 km (radius)Ice and Water Layer: 7500 km thickGas Layer: 9000 km thickTopography: Neptune has no distinct topographical features.Atmosphere: Like the other giant planets, Neptune has a gaseous hydrogen and helium upper layer over a liquid interior. Its blue appearance is due to the presence of methane, which absorbs light in the red and near-infrared wavelengths. Neptune's atmosphere also appears to contain a haze of aerosol particles or ice crystals, the exact composition of which is unknown. The highest wind speeds of any planet 2,400 km (1,500 miles) per hour occur on Neptune. The mean temperature at the cloud tops is -364 F / -220 C / 53 K . The atmosphere on Neptune contains a feature known as the Great Dark Spot, a circular storm the size of Earth that resembles Jupiter's Great Red Spot. The spot spins counter-clockwise and moves west at almost 1,200 km (745 miles) per hour. Magnetic fields and gravity: Neptune's magnetic field is tilted 47 from the planet's rotation axis, and is offset at least 0.55 radii (about 13,500 kilometers or 8,500 miles) from the physical center. The dynamo electric currents produced within the planet, therefore, must be relatively closer to the surface than for Earth, Jupiter or Saturn. The field strength at the surface varies, depending on which hemisphere is being measured, from a maximum of more than 1 gauss in the southern hemisphere to a minimum of less than 0.1 gauss in the northern. (Earth's equatorial magnetic field at the surface is 0.32 gauss.) Because of its unusual orientation and the tilt of the planet's rotation axis, Neptune's magnetic field goes through dramatic changes as the planet rotates in the solar wind. Neptune's magnetic field polarity is the same as those of Jupiter and Saturn, and opposite to that of Earth. The surface gravity of Neptune is 1.22 times the gravity of the Earth.Orbit and rotation: Neptune takes 164.8 years to complete one journey around the Sun. Though a lack of surface detail hinders precise calculation, the equatorial rotation period is believed by some astronomers to be 16 hours. Others believe it to be closer to 22 hours.Moons and/or rings: For many years, there were only two known satellites: Triton and Nereid. In 1987, Voyager 2 provided proof of the existence of 6 more. Triton, by far the largest moon, has a diameter between 6,000 and 7,000 km. (Nereid, the next largest, has a diameter of approximately 500 km.) Triton circles Neptune in a retrograde (backward) orbit and a has tenuous methane atmosphere. The ice caps on Triton are the coldest surface yet found in the solar system (-391 F / -235 C / 2 K). Researchers note that tidal forces on Triton are causing it to spiral toward Neptune. They predict that in 10 to 100 million years, the moon will be so close that Neptune's gravity will tear it apart. Voyager 2 confirmed the existence of the arcs of metallic material surrounding the planet. It was later determined that the arcs were, in fact, thin rings surrounding the planet.Mythology: Neptune is named for the Roman god of the sea, and its astronomical symbol is a trident.Discovery and exploration: Neptune was the first planet to be discovered through mathematical calculation. Its position was predicted in 1845 by English astronomer John Couch Adams and Urbain Jean Joseph LeVerrier of France. In 1846, the planet was identified by Johanne Galle and Heinrich D'Arrest in Berlin. (Both Adams and LeVerrier, however, are credited with the discovery.) Triton was discovered by William Lassell in 1846. Nereid was discovered by G. P. Kuiper in 1949. Modern-day exploration of Neptune was conducted in 1989 by Voyager 2, which came within 4,850 km (3,010 miles) of the planet on August 25.Satellite statistics:Naiad (N3)Mean distance from center of Neptune: 29,960 miles (48,200 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.296 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 0 Diameter: 31 miles (50 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.02 mile (0.03 km) per secondMaximum apparent diameter as seen from Neptune: unknownThalassa (N4)Mean distance from center of Neptune: 31,100 miles (50,000 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.312 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 4.5 Diameter: 56 miles (90 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.025 mile (0.04 km) per secondMaximum apparent diameter as seen from Neptune: unknownDespina (N5)Mean distance from center of Neptune: 32,600 miles (52,500 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.333 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 0 Diameter: 112 miles (180 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.055 mile (0.09 km) per secondMaximum apparent diameter as seen from Neptune: unknownGalatea (N6)Mean distance from center of Neptune: 38,500 miles (62,000 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.429 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 0 Diameter: 100 miles (160 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.045 mile (0.075 km) per secondMaximum apparent diameter as seen from Neptune: unknownLarissa (N7)Mean distance from center of Neptune: 45,700 miles (73,600 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 0.554 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 0 Diameter: 124 miles (200 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.06 mile (0.095 km) per secondMaximum apparent diameter as seen from Neptune: unknownProteus (N8)Mean distance from center of Neptune: 73,090 miles (117,600 km)Inclination of axis: approx. 0 Rotation period: unknownOrbital period: 1.121 daysOrbital eccentricity: 0Orbital inclination to Neptune's equator: 0 Diameter: 260 miles (420 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.12 mile (0.20 km) per secondMaximum apparent diameter as seen from Neptune: unknownTriton (N1)Mean distance from center of Neptune: 220,000 miles (354,800 km)Inclination of axis: 0 Rotation period: 5.877 daysOrbital period: 5.877 daysOrbital eccentricity: 0.0Orbital inclination to Neptune's equator: 157 Diameter: 1,690 miles (2,720 km)Mass: 2.14 x 10^22 kgDensity: 2.07 g/cm^3Escape velocity: 0.9 mile (1.45 km) per secondMaximum apparent diameter as seen from Neptune: 26' 24ΓÇ¥Nereid (N2)Mean distance from center of Neptune: 3,500,000 miles (5,510,000 km)Inclination of axis: unknownRotation period: unknownOrbital period: 360.16 daysOrbital eccentricity: 0.75Orbital inclination to Neptune's equator: 29 Diameter: 210 miles (340 km)Mass: unknownDensity: unknownEscape velocity: approx. 0.11 mile (0.17 km) per secondMaximum apparent diameter as seen from Neptune: 19ΓÇ¥ (average)</text>
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<text>Pluto statisticsDistance from the SunMaximum: 4,583 million miles 7,375 million km 49.19 AUMinimum: 2,766 million miles 4,425 million km 29.69 AUMean: 3,666 million miles 5,900 million km 39.44 AUPeriod of revolution: 247.7 yearsPeriod of rotation (equatorial): 6 days 9 hr.Mean orbital velocity: 2.9 miles (4.7 km) per secondInclination of axis: 122.5 Orbital eccentricity: 0.248Orbital inclination: 17.15 Diameter at equator: 1,430 miles (2,300 km) 0.192 x Earth's diameterOblateness: 0Mass: 1.29 x 10^22 kg 0.002 x Earth's massVolume: 1.08 x 10^10 km^3 0.01 x Earth's volumeDensity: 2.03 g/cm^3 0.85 x Earth's densitySurface gravity: 0.4 m/s^2 0.04 x Earth's gravityEscape velocity: 0.7 miles (1.1 km) per secondMean surface temperature: -382 F / -230 C / 43 KMaximum apparent diameter as seen from Earth: 0.2"Albedo: 0.4Number of known satellites: 1Mean diameter of Sun as seen from the planet: 49"Satellite statisticsCharonMean distance from center of Pluto: 12,200 miles (19,600 km)Inclination of axis: 0 Rotation period: 6.39 daysOrbital period: 6.39 daysOrbital eccentricity: lowOrbital inclination to Pluto's equator: 98.80Diameter: 745 miles (1,200 km)Mass: 1.77 x 1021 kgDensity: 2 g/cm3Escape velocity: 0.37 mile (0.59 km) per secondPlanet compositionLittle is known about the composition of Pluto, but its low density (about twice that of water) indicates a major constituent must be methane and water ice. The remainder is probably silicate rock, perhaps in a core surrounded by an icy mantle. Although no clear surface detail has been seen on Pluto, there appears to be a dark band near its equator.Pluto's diameter is about 2,300 km (2/3 the size of our moon); Charon's is approximately 1200 km. The two are so close in size that they are sometimes called a "double planet."Together, Pluto and Charon have about 1/5 the mass of our Moon.TopographyNo surface detail has been detected on either Pluto or its satellite, Charon.AtmosphereUntil 1988 it was not known if Pluto had an atmosphere. In that year, an occultation of a star by Pluto was observed. Because the star gradually disappeared behind Pluto instead of instantaneously, it was determined that Pluto did in fact have atmosphere. This atmosphere blocked part of the star's light before the planet blocked all of it. Had there been no atmosphere, the star would have stayed a constant brightness until it was behind Pluto.This tenuous atmosphere is probably pure methane; the surface pressure on Pluto is about 100,000 times less than the pressure at sea level on Earth. It is possible that very high in the atmosphere is a "smoggy" region of ammonia, methane and other hydrocarbons, and carbon monoxide.Magnetic fields and gravityThere is no reason to believe Pluto has an inherent magnetic field because it probably lacks an iron core. However, it is likely that there are interactions of some sort between the solar wind and Pluto's surface or atmosphere.Pluto's surface gravity estimated to be around 0.08 times that of the Earth.Orbit and rotationIt takes 248 years for Pluto to complete an orbit of the Sun. Its equatorial rotation is 6.3 days.At 17, Pluto has the most highly-inclined orbit of all planets. Pluto also has the most eccentric orbit. This eccentricity takes Pluto inside Neptune's orbit, where it has been since 1977 and will remain until March 1999.Moons (and/or rings)The only known satellite is Charon, which orbits Pluto every 6.3 days. Charon appears to be covered in water ice (as opposed to the methane ice that covers Pluto). Charon's orbit is locked with Pluto's, so the same sides of the globes always face each other.MythologyPluto was named for the Greek god of the lower world.Discovery and explorationClyde Tombaugh discovered Pluto in January 1930 based on calculations and predictions made by Percival Lowell at the turn of the century. James Christy first speculated about the existence of Pluto's satellite, Charon, in 1978. The Hubble Space Telescope later verified its existence. Pluto is the only major body in our solar system that has not been visited by an exploratory probe, but NASA is currently exploring the possibility of such a probe.</text>
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<text><span class="style2">unPlanet statisticsPeriod of revolution ("one year"): N/APeriod of rotation (as seen from Earth):26.8 daysMean orbital velocity per second (in millions):N/AInclination of axis: unknownOrbital eccentricity: N/AOrbital inclination: N/ADiameter at equator: unknown miles (1,392,530 km)Escape velocity per second: unknown mphMean temperature: Core: 27,000,000  F / 15,000,000 C / 15,000,000 KSurface: 10,000  F / 5,500 C / 5,500 KMass (Earth = 1): 1.9891x1030 kgVolume (Earth =1):1.414 x 1027 m3Density (water = 1):Entire sun 1,410 kgm m-3Interior (center)1.6 x 105 kg m -3Surface gravity (Earth = 1): unknownMaximum apparent diameter as seen from Earth (seconds of arc): unknownPlanet compositionThe Sun, which is really a star, dwarfs the other planetary bodies. It represents approximately 99.86 percent of all the mass in the solar system. All of the planets, moons, asteroids, comets, dust, and gas add up to only about 0.14% of the mass of the Sun. This 0.14% represents the material left over from the Sun's formation. One hundred nine Earth's would fit side-by-side across the Sun's disk, and its interior could hold 1.3 million Earth's.The visible surface of the sun is known as the photosphere ("sphere of light"). The photosphere is a shell of gas about 400 km thick. With the exception of a tiny fraction, all of the Sun's light is emitted from a 100 km thick slice of the photosphere. The photosphere is covered by the chromosphere, which is several thousands of kilometers thick. That, in turn, is overlaid by the region known as the corona, which is generally about 200 km thick. Beyond that layer lies the magnetosphere and the solar wind.TopographyThe chromosphere of the Sun (considered to be the surface) changes rapidly. There are, however, several frequent phenomenon that could be considered topographical features of the Sun.The edge of the sun appears to be made up of many flame-like protrusions, known as spicules. Spicules are vertical columns of gas that follow the directions of the local magnetic fields and rise to about 10,000 km. They typically have temperatures ranging from 10,000 to 20,000 K. The average spicule lasts from 5 to 10 minutes.A longer-lived version of the spicule is known as a prominence. Prominences appear in the upper chromosphere and inner corona as flame-like clouds. Some (known as quiescent prominences) maintain their form and volume for as much as a full year before breaking up and disappearing. The mass of a prominence is about 100 times greater than the surrounding material, but the temperature is much lower. Though they seem to be comprised of material surging up from the chromosphere, the great majority consist of material condensing from the corona and flowing downward. The Sun also exhibits sun spots, which consist of a dark central region (the umbra) surrounded by a lighter region (the penumbra). On the whole, these spots are relatively cool. Although there is no completely satisfactory theory on the origin of sunspots, the Babcock-Leighton theory has gained the greatest acceptance.Magnetic field and gravityThe Sun produces a strong magnetic field and streams of charged particles (known as solar wind), both of which extend far beyond the planets. The magnetic field strength varies according to the location and feature being measured: Sunspots exert 3,000G; polar fields 5G; prominences 10 to 100G; and chromospheric plages 200G.Orbit and rotationBecause it is the center of our solar system, the Sun does not have an orbit. It does, however, rotate once on its axis every 26.8 days.MythologyFor many years, people thought the Earth was the center of our universe (as described by the theory made famous by Claudius Ptolemy). People also believed that the Sun was the creator of the Earth and dispensed all light, life, and power. The Sun, in essence, was the king and many civilizations developed rituals to honor the deity (such as the Christian habit of resting on Sunday).Discovery and explorationMany spacecraft have explored the Sun's environment, but none have gotten any closer to its surface than approximately two-thirds the distance from Earth to the Sun. Pioneers 5 - 11, the Pioneer Venus Orbiter, Voyagers, 1 and 2, and other spacecraft have all sampled the solar environment. The Ulysses spacecraft, launched October 6, 1990 as a joint solar mission of NASA and the European Space Agency, will fly over the Sun's polar regions during 1994 and 1995 to perform a wide range of experiments.</span></text>
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<text>By far the largest member of the Solar System is the Sun, which contains over 99% of the total mass of the Solar System. The planets Mercury, Venus, Earth, and Mars are small, rocky worlds relatively close to the Sun. The giant gaseous planets, Jupiter, Saturn, Uranus, and Neptune, are considerably larger and are further from the Sun. The last planet, Pluto, is small and cold. Sharing the Solar System with the planets are the much smaller asteroids and comets.The Sun is a star, one of the 100 billion that constitute our galaxy, the Milky Way. The stars in the Milky Way are grouped into a spherical shape at the center of the galaxy, and a thin disk around it; the Sun and the Solar System are located in the disk, over 10^17 km from the center. Just like the planets orbit the Sun, the Sun and the entire Solar System orbit the center of the galaxy every 240 million years. Our Sun is not unusual; there are many stars like it in the Milky Way. For this reason, many scientists believe other stars in the galaxy may have planets of their own, perhaps even planets bearing other forms of life. </text>
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<script>on openCardglobal printFieldlock screencolorizeHC "Add","PLANETS:GRAPHICS:SUMM.PIC"unlock screennoPaintWhiteif there is a window "options"thenhide window "options"if there is a cd fld printField then hide cd fld printFieldelsepass openCardend ifend ifshow cd field printFieldend openCardon idlenoPaintWhitehide menuBarend idleon goOptionslock screengo backunlock screenend goOptionson closeCardlock screenglobal switch, printFieldput 1 into switchhide cd field printFieldcolorizeHC "colorFill" -- redraw previous screensunlock screenhide menuBarend closeCard</script>
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card_2840.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<script>on mouseUpglobal xadd 1 to xlock screenif x = 1thencolorizeHC "Add","PLANETS:GLOSSARY:SOURCES:S2.PIC", "60,38,580,336"elseif x = 2thencolorizeHC "Add","PLANETS:GLOSSARY:SOURCES:S3.PIC", "60,38,580,336"elseif x = 3thencolorizeHC "Add","PLANETS:GLOSSARY:SOURCES:S1.PIC", "60,38,580,336"end ifend ifif x > 3 then put 0 into xend ifunlock screenend mouseUp</script>
<script>on mouseDownglobal choice, compareOthersput the clickLine into choicecompareAscompareBscompareCscompareDscompareEscompareFscompareGscompareHscompareIscompareJscompareKscompareLscompareMs --midway of checkercompareOthersend mouseDownon compareAsglobal term, choice, thePictureif choice = "line 1 of card field 1"thenput "G001.PIC" into term --Absolute zeroput "G001.PIC" into thePictureshoTermelseif choice = "line 2 of card field 1"thenput "G002.PIC" into termput "G002.PIC" into thePictureshoTermelseif choice = "line 3 of card field 1"thenput "G003.PIC" into termput "G003.PIC" into thePictureshoTermelseif choice = "line 4 of card field 1"thenput "G004.PIC" into termput "G004.PIC" into thePictureshoTermelseif choice = "line 5 of card field 1"thenput "G005.PIC" into termput "G005.PIC" into thePictureshoTermelseif choice = "line 6 of card field 1"thenput "G006.PIC" into termput "G006.PIC" into thePictureshoTermelseif choice = "line 7 of card field 1"thenput "G007.PIC" into termput "G007.PIC" into thePictureshoTermelseif choice = "line 8 of card field 1"thenput "G008.PIC" into termput "G008.PIC" into thePictureshoTermelseif choice = "line 9 of card field 1"thenput "G009.PIC" into termput "G009.PIC" into thePictureshoTermelseif choice = "line 10 of card field 1"thenput "G010.pic" into termput "G010.pic" into thePictureshoTermQTMovie OpenMovie,Plain,"PLANETS:GLOSSARY:11GLO.AVI", "256,72",¬nocontroller,dontPaintWhite,loopend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend compareAson compareBsglobal term, choice, thePictureif choice = "line 11 of card field 1"thenput "G011.PIC" into termput "G011.PIC" into thePictureshoTermelseif choice = "line 12 of card field 1"thenput "G012.PIC" into termput "G012.PIC" into thePictureshoTermelseif choice = "line 13 of card field 1"thenput "G013.PIC" into termput "G013.PIC" into thePictureshoTermend ifend ifend ifend compareBson compareCsglobal term, choice, thePictureif choice = "line 14 of card field 1"thenput "G014.PIC" into termput "G014.PIC" into thePictureshoTermelseif choice = "line 15 of card field 1"thenput "G015.PIC" into termput "G015.PIC" into thePictureshoTermelseif choice = "line 16 of card field 1"thenput "G016.PIC" into termput "G016.PIC" into thePictureshoTermelseif choice = "line 17 of card field 1"thenput "G017.PIC" into termput "G017.PIC" into thePictureshoTermelseif choice = "line 18 of card field 1"thenput "G018.PIC" into termput "G018.PIC" into thePictureshoTermelseif choice = "line 19 of card field 1"thenput "G019.PIC" into termput "G019.PIC" into thePictureshoTermelseif choice = "line 20 of card field 1"thenput "G020.PIC" into termput "G020.PIC" into thePictureshoTermelseif choice = "line 21 of card field 1"thenput "G021.PIC" into termput "G021.PIC" into thePictureshoTermelseif choice = "line 22 of card field 1"thenput "G022.PIC" into termput "G022.PIC" into thePictureshoTermelseif choice = "line 23 of card field 1"thenput "G023.PIC" into termput "G023.PIC" into thePictureshoTermelseif choice = "line 24 of card field 1"thenput "G024.PIC" into termput "G024.PIC" into thePictureshoTermelseif choice = "line 25 of card field 1"thenput "G025.PIC" into termput "G025.PIC" into thePictureshoTermelseif choice = "line 26 of card field 1"thenput "G026.PIC" into termput "G026.PIC" into thePictureshoTermelseif choice = "line 27 of card field 1"thenput "G027.PIC" into termput "G027.PIC" into thePictureshoTermelseif choice = "line 28 of card field 1"thenput "G028.PIC" into termput "G028.PIC" into thePictureshoTermelseif choice = "line 29 of card field 1"thenput "G029.PIC" into termput "G029.PIC" into thePictureshoTermend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend compareCson compareDsglobal term, choice, thePictureif choice = "line 30 of card field 1"thenput "G030.PIC" into termput "G030.PIC" into thePictureshoTermelseif choice = "line 31 of card field 1"thenput "G031.PIC" into termput "G031.PIC" into thePictureshoTermelseif choice = "line 32 of card field 1"thenput "G032.PIC" into termput "G032.PIC" into thePictureshoTermelseif choice = "line 33 of card field 1"thenput "G033.PIC" into termput "G033.PIC" into thePictureshoTermend ifend ifend ifend ifend compareDson compareEsglobal term, choice, thePictureif choice = "line 34 of card field 1"thenput "G034.PIC" into termput "G034.PIC" into thePictureshoTermelseif choice = "line 35 of card field 1"thenput "G035.PIC" into termput "G035.PIC" into thePictureshoTermelseif choice = "line 36 of card field 1"thenput "G036.PIC" into termput "G036.PIC" into thePictureshoTermelseif choice = "line 37 of card field 1"thenput "G037.PIC" into termput "G037.PIC" into thePictureshoTermelseif choice = "line 38 of card field 1"thenput "G038.PIC" into termput "G038.PIC" into thePictureshoTermelseif choice = "line 39 of card field 1"thenput "G039.PIC" into termput "G039.PIC" into thePictureshoTermelseif choice = "line 40 of card field 1"thenput "G040.PIC" into termput "G040.PIC" into thePictureshoTermelseif choice = "line 41 of card field 1"thenput "G041.PIC" into termput "G041.PIC" into thePictureshoTermelseif choice = "line 42 of card field 1"thenput "G042.PIC" into termput "G042.PIC" into thePictureshoTermelseif choice = "line 43 of card field 1"thenput "G043.PIC" into termput "G043.PIC" into thePictureshoTermelseif choice = "line 44 of card field 1"thenput "G044.PIC" into termput "G044.PIC" into thePictureshoTermelseif choice = "line 45 of card field 1"thenput "G045.PIC" into termput "G045.PIC" into thePictureshoTermend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend compareEson compareFsglobal term, choice, thePictureif choice = "line 46 of card field 1"thenput "G046.PIC" into termput "G046.PIC" into thePictureshoTermelseif choice = "line 47 of card field 1"thenput "G047.PIC" into termput "G047.PIC" into thePictureshoTermelseif choice = "line 48 of card field 1"thenput "G048.PIC" into termput "G048.PIC" into thePictureshoTermend ifend ifend ifend compareFson compareGsglobal term, choice, thePictureif choice = "line 49 of card field 1"thenput "G049.PIC" into termput "G049.PIC" into thePictureshoTermelseif choice = "line 50 of card field 1"thenput "G050.PIC" into termput "G050.PIC" into thePictureshoTermelseif choice = "line 51 of card field 1"thenput "G051.PIC" into termput "G051.PIC" into thePictureshoTermelseif choice = "line 52 of card field 1"thenput "G052.PIC" into termput "G052.PIC" into thePictureshoTermelseif choice = "line 53 of card field 1"thenput "G053.PIC" into termput "G053.PIC" into thePictureshoTermelseif choice = "line 54 of card field 1"thenput "G054.PIC" into termput "G054.PIC" into thePictureshoTermelseif choice = "line 55 of card field 1"thenput "G055.PIC" into termput "G055.PIC" into thePictureshoTermelseif choice = "line 56 of card field 1"thenput "G056.PIC" into termput "G056.PIC" into thePictureshoTermelseif choice = "line 57 of card field 1"thenput "G057.PIC" into termput "G057.PIC" into thePictureshoTermelseif choice = "line 58 of card field 1"thenput "G058.PIC" into termput "G058.PIC" into thePictureshoTermend ifend ifend ifend ifend ifend ifend ifend ifend ifend ifend compareGson compareHsglobal term, choice, thePictureif choice = "line 59 of card field 1"thenput "G059.PIC" into termput "G059.PIC" into thePictureshoTermelseif choice = "line 60 of card field 1"thenput "G060.PIC" into termput "G060.PIC" into thePictureshoTermelseif choice = "line 61 of card field 1"thenput "G061.PIC" into termput "G061.PIC" into thePictureshoTermend ifend ifend ifend compareHson compareIsglobal term, choice, thePictureif choice = "line 62 of card field 1"thenput "G062.PIC" into termput "G062.PIC" into thePictureshoTermelseif choice = "line 63 of card field 1"thenput "G063.PIC" into termput "G063.PIC" into thePictureshoTermelseif choice = "line 64 of card field 1"thenput "G064.PIC" into termput "G064.PIC" into thePictureshoTermend ifend ifend ifend compareIson compareJsglobal term, choice, thePictureif choice = "line 65 of card field 1"thenput "G065.PIC" into termput "G065.PIC" into thePictureshoTermend ifend compareJson compareKsglobal term, choice, thePictureif choice = "line 66 of card field 1"thenput "G066.PIC" into termput "G066.PIC" into thePictureshoTermelseif choice = "line 67 of card field 1"thenput "G067.PIC" into termput "G067.PIC" into thePictureshoTermelseif choice = "line 68 of card field 1"thenput "G068.PIC" into termput "G068.PIC" into thePictureshoTermend ifend ifend ifend compareKson compareLsglobal term, choice, thePictureif choice = "line 69 of card field 1"thenput "G069.PIC" into termput "G069.PIC" into thePictureshoTermelseif choice = "line 70 of card field 1"thenput "G070.PIC" into termput "G070.PIC" into thePictureshoTermelseif choice = "line 71 of card field 1"thenput "G071.PIC" into termput "G071.PIC" into thePictureshoTermelseif choice = "line 72 of card field 1"thenput "G072.PIC" into termput "G072.PIC" into thePictureshoTermelseif choice = "line 73 of card field 1"thenput "G073.PIC" into termput "G073.PIC" into thePictureshoTermelseif choice = "line 74 of card field 1"thenput "G074.PIC" into termput "G074.PIC" into thePictureshoTermend ifend ifend ifend ifend ifend ifend compareLson compareMsglobal term, choice, thePictureif choice = "line 75 of card field 1"thenput "G075.PIC" into termput "G075.PIC" into thePictureshoTermelseif choice = "line 76 of card field 1"thenput "G076.PIC" into termput "G076.PIC" into thePictureshoTermelseif choice = "line 77 of card field 1"thenput "G077.PIC" into termput "G077.PIC" into thePictureshoTermelseif choice = "line 78 of card field 1"thenput "G078.PIC" into termput "G078.PIC" into thePictureshoTermelseif choice = "line 79 of card field 1"thenput "G079.PIC" into termput "G079.PIC" into thePictureshoTermelseif choice = "line 80 of card field 1"thenput "G080.PIC" into termput "G080.PIC" into thePictureshoTermelseif choice = "line 81 of card field 1"thenput "G081.PIC" into termput "G081.PIC" into thePictureshoTermelseif choice = "line 82 of card field 1"thenput "G082.PIC" into termput "G082.PIC" into thePictureshoTermelseif choice = "line 83 of card field 1"thenput "G083.PIC" into termput "G083.PIC" into thePictureshoTermend ifend ifend ifend ifend ifend ifend ifend ifend ifend compareMs</script>
</part>
<part>
<id>41</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>496</left>
<top>350</top>
<right>565</right>
<bottom>367</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>cancel</name>
<script>on mouseUpglobal thePicture, checkMoviescheckMoviesif there is a window thePicturethennoPaintWhiteclose window thePictureend ifresetSystemPaletteloadPalettecolorizeHC "Add","PLANETS:GRAPHICS:GLOS.PIC"noPaintWhitesendBackend mouseUpon checkMoviesnoPaintWhiteif there is a window "11GLO.AVI" then close window "11GLO.AVI"if there is a window "108GLO.AVI" then close window "108GLO.AVI"end checkMovieson sendBacklock screengo backunlock screenend sendBack</script>
</part>
<content>
<layer>card</layer>
<id>38</id>
<text>Absolute zeroAccretionAdvectionAlbedoAphelionApogeeAsteroidAtmosphereAuroraAxisBarycenterBedrockBow shockCalderaCassini DivisionCelestial EquatorCelestial SphereChromosphereComaCometConjunctionConstellationContinental DriftConvectionCopernican SystemCoriolis ForceCoronaCosmic raysCrustDayDeclinationDensityDynamoEccentricityEclipseEclipticEcosphereElectromagnetic spectrumEllipseElongationEphemerisEquatorEquinoxEscape velocityExosphereFaculaeFlocculiFusionGalaxyGamma raysGeocentricGeodesyGibbousGrabenGravityGreat CircleGreenhouse EffectGreenwich Mean Time (GMT)HaloHeliocentricHemisphereInclinationInfrared radiationIonosphereJovian PlanetsKepler's Laws of Planetary MotionKirkwood gapsKuiper Belt or Kuiper CloudLagrangian PointsLatitudeLight-yearLimbLithosphereLongitudeMagnetic stormMagnetosphereMagnitudeMantleMassMeridianMeteoroidsMicronMillibarNadirOblatenessObliquityOort CloudOppositionOrbitOrbital ResonanceParallaxParsecPenumbraPerigeePerihelionPhasesPhotospherePlanetPlanet XPlanetesimalPlasmaPrecessionPrograde MotionProminencePtolemaic SystemRadial velocityRadianRadiationRegolithRetrograde MotionRevolutionRight AscensionRoche LimitRotationSatelliteScientific NotationSelenographySidereal MonthSidereal PeriodSolar SystemSolar WindSolsticeSpecific gravitySpin-Orbit CouplingStarStar Black holeStar Main sequence starStar Neutron star/PulsarStar Other Types Star Red giantStar SupernovaStar White dwarfStar catalogueStratosphereSunspotSynchronous RotationSynodic PeriodTelemetryTelescopeTerminatorTidal ForceTideTransfer orbitTransitTrojan asteroidsTroposphereTychonic SystemUltraviolet radiationUmbraUnits of Measure PrefixesUnits of Measure Angular unitsUnits of Measure LengthUnits of Measure PressureUnits of Measure Speed of lightUnits of Measure Speed of soundUnits of Measure TemperatureUniverseVan Allen Zones (or Belts)VulcanWeightZenithZodiac</text>
</content>
<name>GLOSSARY</name>
<script>on openCardlock screencolorizeHC "Add","PLANETS:GRAPHICS:GLOS.PIC"unlock screenshow cd field "A"end openCardon shoTerm picTermglobal term, thePictureput "PLANETS:GLOSSARY:TERMS_MAC:"&term&"" into picTermlock screennoPaintWhitepicture picTerm,file,rect,false,8set loc of window thePicture to "60,39" --test the locationnoPaintWhiteshow window thePicturenoPaintWhiteunlock screenend shoTermon closeCardglobal switch, thePicturespinCursorlock screencolorizeHC "colorFill" -- redraw previous screensunlock screennoPaintWhiteput 1 into switchif there is a window thePicture then close window thePictureend closeCardon bHilite theButton, width-- hilite a button with a variable-width frame.-- rej 1/23/94----------------put the rect of theButton into temp-- calculate a smaller rect.put quote & item 1 of temp + width & comma & item 2 of temp + width & ¬comma & item 3 of temp - width & comma & item 4 of temp - width & ¬quote into temp2-- set clipping region to exclude the smaller rect.QTPict DiffClip, temp2-- now highlight button - smallrect, leaving frame.set the hilite of theButton to truerepeat until the mouse is up-- do TrackWithin equivalent as long as the mouse is down.-- conditionals may seem redundant but are designed to-- eliminate unnecessary param sets.if the MouseLoc is within temp thenif not the hilite of theButton thenset the hilite of theButton to trueend ifelseif the hilite of theButton thenset the hilite of theButton to falseend ifend ifend repeatwait 4 ticks -- to get a nice flash. Otherwise it may be too quick to see if just tapped.if the hilite of theButton thenset the hilite of theButton to falseend ifQTPict ClipTo, "0,0,2400,2400"end bHiliteon frameHilite -- hilite a clicked button or field, call-- from mouseDown script with no params. Default setup for bHilite.----------------bHilite the target, 2play "mouseClick"end frameHiliteon checkMoviesglobal thePicturenoPaintWhiteif there is a window "11GLO.AVI" then close window "11GLO.AVI"noPaintWhiteif there is a window "108GLO.AVI" then close window "108GLO.AVI"noPaintWhiteif there is a window thePicture then close window thePictureend checkMovieson goGlosslock screengo backunlock screenend goGloss</script>
</card>
card_5619.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<script>on openCardglobal movieID-- noPaintWhite-- hide window "runMenu"noPaintWhiteif there is a window "black" then ¬close window "black"lock screencolorizeHC "Add","PLANETS:GRAPHICS:INTRO.PICT"unlock screenQTMovie OpenMovie,Direct,"PLANETS:GRAPHICS:INTRO Final.Moov","124,211",invisibleput the result into movieIDQTMovie Direct, movieID,Play,HideController,closeOnFinishQTMovie Direct,movieID,Get,Currtimeput the result into startTimeQTMovie Direct,movieID,Get,durationput the result into duration-- put startTime + duration into endTimeput 18230 into endTimeQTMovie Direct,movieID,PlayrepeatQTMovie Direct,movieID,Get,Currtimeput the result into tempif (temp >= endTime) or (the mouse is down) thenQTMovie Direct, movieID, Disposeexit repeatelseQTMovie Direct,movieID,idleend ifend repeatgo card 1end openCardon closeCardglobal movieID, introSwitchQTMovie Direct, movieID, Disposelock screennoPaintWhiteprepWinnoPaintWhiteif there is a window "runMenu"thenshow window "runMenu"elseloadPaletteend ifunlock screenput 0 into introSwitchend closeCard</script>
</card>
card_2156.xml
<?xml version="1.0" encoding="utf-8" ?>
<!DOCTYPE card PUBLIC "-//Apple, Inc.//DTD card V 2.0//EN" "" >
<script>on mouseDownlock Screenplay "mouseClick"go to stack "PLANETS:MARS:MARS.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "marPic"thennoPaintWhiteshow window "marPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "marPic"thennoPaintWhitehide window "marPic"end ifend mouseLeave</script>
</part>
<part>
<id>2</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>271</left>
<top>231</top>
<right>290</right>
<bottom>252</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>venus</name>
<script>on mouseDownplay "mouseClick"lock Screengo to stack "PLANETS:VENUS:VENUS.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "venPic"thennoPaintWhiteshow window "venPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "venPic"thennoPaintWhitehide window "venPic"end ifend mouseLeave</script>
</part>
<part>
<id>5</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>369</left>
<top>229</top>
<right>389</right>
<bottom>252</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>earth</name>
<script>on mouseDownlock Screengo to stack "PLANETS:EARTH:EARTH.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "earPic"thennoPaintWhiteshow window "earPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "earPic"thennoPaintWhitehide window "earPic"end ifend mouseLeave</script>
</part>
<part>
<id>6</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>420</left>
<top>230</top>
<right>496</right>
<bottom>308</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>jupiter</name>
<script>on mouseDownlock Screengo to stack "PLANETS:JUPITER:JUPITER.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "jupPic"thennoPaintWhiteshow window "jupPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "jupPic"thennoPaintWhitehide window "jupPic"end ifend mouseLeave</script>
</part>
<part>
<id>7</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>335</left>
<top>230</top>
<right>348</right>
<bottom>244</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>mercury</name>
<script>on mouseDownlock Screengo to stack "PLANETS:MERCURY:MERCURY.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "merPic"thennoPaintWhiteshow window "merPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "merPic"thennoPaintWhitehide window "merPic"end ifend mouseLeave</script>
</part>
<part>
<id>8</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>317</left>
<top>45</top>
<right>334</right>
<bottom>65</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>pluto</name>
<script>on mouseDownlock Screengo to stack "PLANETS:PLUTO:PLUTO.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "pluPic"thennoPaintWhiteshow window "pluPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "pluPic"thennoPaintWhitehide window "pluPic"end ifend mouseLeave</script>
</part>
<part>
<id>9</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>105</left>
<top>280</top>
<right>247</right>
<bottom>369</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>saturn</name>
<script>on mouseDownlock Screengo to stack "PLANETS:SATURN:SATURN.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "satPic"thennoPaintWhiteshow window "satPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "satPic"thennoPaintWhitehide window "satPic"end ifend mouseLeave</script>
</part>
<part>
<id>10</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>317</left>
<top>168</top>
<right>332</right>
<bottom>184</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>neptune</name>
<script>on mouseDownlock Screengo to stack "PLANETS:NEPTUNE:NEPTUNE.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "nepPic"thennoPaintWhiteshow window "nepPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "nepPic"thennoPaintWhitehide window "nepPic"end ifend mouseLeave</script>
</part>
<part>
<id>11</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>66</left>
<top>195</top>
<right>85</right>
<bottom>216</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>uranus</name>
<script>on mouseDownlock Screengo to stack "PLANETS:URANUS:URANUS.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "uraPic"thennoPaintWhiteshow window "uraPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "uraPic"thennoPaintWhitehide window "uraPic"end ifend mouseLeave</script>
</part>
<part>
<id>13</id>
<type>button</type>
<visible> <true /> </visible>
<reserved5> 0 </reserved5>
<reserved4> 0 </reserved4>
<reserved3> 0 </reserved3>
<reserved2> 0 </reserved2>
<reserved1> 0 </reserved1>
<enabled> <true /> </enabled>
<rect>
<left>308</left>
<top>227</top>
<right>332</right>
<bottom>254</bottom>
</rect>
<style>transparent</style>
<showName> <false /> </showName>
<highlight> <false /> </highlight>
<autoHighlight> <false /> </autoHighlight>
<sharedHighlight> <true /> </sharedHighlight>
<family>0</family>
<titleWidth>0</titleWidth>
<icon>0</icon>
<textAlign>center</textAlign>
<font>Chicago</font>
<textSize>12</textSize>
<textStyle>plain</textStyle>
<name>SUN</name>
<script>on mouseDownbreakMovielock Screengo to stack "PLANETS:SUN:SUN.HC"unlock Screenend mouseDownon mouseWithinsolarTitleOffif there is a window "sunPic"thennoPaintWhiteshow window "sunPic"end ifend mouseWithinon mouseLeavesolarTitleOnif there is a window "sunPic"thennoPaintWhitehide window "sunPic"end ifend mouseLeave</script>
<script>on openCardglobal introSwitchspinCursorlock screencolorizeHC "Add","PLANETS:GRAPHICS:SOLAR.PIC"unlock screenpicture "marPic",resource,rect,false,8set rect of window "marPic" to "215,211,263,222"picture "earPic",resource,rect,false,8set rect of window "earPic" to "364,210,421,221"picture "venPic",resource,rect,false,8set rect of window "venPic" to "260,217,320,227"picture "satPic",resource,rect,false,8set rect of window "satPic" to "141,259,213,270"picture "jupPic",resource,rect,false,8set rect of window "jupPic" to "428,201,502,212"picture "nepPic",resource,rect,false,8set rect of window "nepPic" to "295,145,376,155"picture "merPic",resource,rect,false,8set rect of window "merPic" to "310,200,394,209"picture "uraPic",resource,rect,false,8set rect of window "uraPic" to "55,178,126,189"picture "pluPic",resource,rect,false,8set rect of window "pluPic" to "301,37,357,46"picture "sunPic",resource,rect,false,8set rect of window "sunPic" to "304,214,341,225"picture "solPic",resource,rect,false,8set rect of window "solPic" to "492,24,631,35"noPaintWhiteshow window "solPic"show window "runMenu"end openCardon idleglobal introSwitchnoPaintWhiteif there is a window "black"thenclose window "black"if introSwitch < 1 thenplay "WelcomeAudio.AIFF"end ifend ifput 1 into introSwitchend idleon closeCardlock screenglobal switch, introSwitchbreakMovienoPaintWhiteif there is a window "marPic" then ¬close window "marPic"if there is a window "earPic" then ¬close window "earPic"if there is a window "venPic" then ¬close window "venPic"if there is a window "satPic" then ¬close window "satPic"if there is a window "jupPic" then ¬close window "jupPic"if there is a window "nepPic" then ¬close window "nepPic"if there is a window "merPic" then ¬close window "merPic"if there is a window "uraPic" then ¬close window "uraPic"if there is a window "pluPic" then ¬close window "pluPic"if there is a window "sunPic" then ¬close window "sunPic"if there is a window "solPic" then ¬close window "solPic"colorizeHC "colorFill" -- redraw previous screensunlock screenpointerput 0 into switchput 1 into introSwitchend closeCardon solarTitleOffif there is a window "solPic"thennoPaintWhitehide window "solPic"end ifend solarTitleOffon solarTitleOnif there is a window "solPic"thennoPaintWhiteshow window "solPic"end ifend solarTitleOnon mouseDownlock screengo to stack "PLANETS:SOLAR:SOLAR.HC"unlock screenend mouseDown</script>
 (1994).iso/mac/Journey to the Planets/Journey to the Planets/BMAP_3612.png){kind=link}
 (1994).iso/mac/Journey to the Planets/Journey to the Planets/PATs.png){kind=link}