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OurSolarSystem Joe Korczynski 09-26-93 New... Open... Make Copy... Streamline... Print... Report... Preferences... Workbench Help... About... Quit... Paste Clear Select All Cut Page Copy Page Colors Load... Save... Restore Colors Default Colors Brush Colors Image Colors Cycle Grid... Stop Sound Show All Unlock All Edit Form Share Next Page Previous Page First Page Last Page Backward Forward Last Book Browse... Autobrowse... Bookshelf New Page Delete Page New Form Load Form... Save Form... Image Load... Save... Capture... Clipboard Paste Spare Swap Frames Copy to Spare Merge in Front Merge in Back Delete Spare Frame Previous Delete Copy to All Color Remap Transparency Paper <-> Pen Paper -> Pen Count Vertical Horizontal Info... Brush Load... Save... 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Effect Area earth.iff HelveticaN39 jupiter.iff mars.iff mercury.iff neptune.iff pluto.iff saturn.iff solarchart-1 topaz11 uranus.iff venus.iff topaz.font helvetica.font HelveticaN.font times.font thinpaz.font Palatino.font Pica.font Solar-Page Info-Page Mercury-Page Venus-Page Earth-Page Mars-Page Jupitor-Page Saturn-Page Uranus-Page Neptune-Page Pluto-PagePREF %HD2:Brilliance-Documents/solarchart-1 HD0:Fonts-Scala/HelveticaN/39 planets #Data:Brilliance-Documents/pluto.iff $Data:Brilliance-Documents/solarchart Info-Form Mean Distance From Sun: Mean Orbital Velocity: Length of Year: Length of Day: Diameter: Number of Known Satellites: Mass: Planet_Info Planet_Name (Click Here To Return To Our Solar System <<<UUUdddttt MERCURY E Once Mercury was thought to be the littlest, hottest planet, and @scientists believed that is kept one face always toward the Sun. BSpacecraft, radar and telescopic observations have disproved those Cerstwhile "facts;" they have also revealed new mysteries about this Hsmall world closest to the Sun. While Pluto is the littlest and Venus is Gthe hottest, Nercury is the densest planet, with its interior dominated Gby a huge iron core. Evidently the core is partly molten, since it must Eact like a dynamo to generate Mercury's weak, but Earthlike, magnetic Cfield. It is suprising that the core's heat has not all leaked into Cspace through Mercury's thin mantle; it is also difficult to fathom Ddynamo action inside such a slowly rotating body ( Mercury's spin is 0exactly two-thirds of its 88-day orbital year ). F Scientists once thought Mercury to be nearly a carbon-copy of our HMoon, but that's not true! Gently rolling intercrater plains distinguish Hits surface and its surface reflectivity is different. Mercury is unique Din being crisscrossed by enormous thrust faults formed as the planet Dcontracted while it cooled. Although Mercury's atmosphere -- perhaps Grelated to the solar wind sometimes reaching the planet's surface -- is Gtenuous, many scientists were surprised that Mercury has any atmosphere at all. D In many ways, Mercury is at our near the end of the spectrum of ?planetary properties: in solar distance, composition, dynamical Fproperties, size and environmental conditions. It is a fascinating, if Ginhospitable planet, difficult to glimpse from Earth as it hides in the ?Sun's glare, but available for follow-up studies by technically Jadvanced, heat-resistant spacecraft. Clark R. Chapman, Planetary Science :Institute, Science Applications International Corporation. Mass: 0.0558 Earth-mass Number of Satellites: 0 Diameter: 4,878 km Length of Day: 58.6 Earth-days "Length of Year: 0.2408 Earth-years #Mean Orbital Velocity: 47.89 km/sec "Mean Distance From Sun: 57.9 E6 km Mercury-Page VENUS B Venus has often been called Earth's sister world, for the two Bplanets are about the same size and orbit in the same neighborhood Cof the solar system. But spacecraft, and Earth-based investigations @have revealed Venu as a very different world. The planet rotates Aabout its axis in a retrograde direction (opposite to its orbital ?direction), and its day is equal to 243 Earth-days, longer than its year. Q Venus' thick atmosphere is composed of carbon dioxide (CO Bwith clouds of sulfuric acid. Winds in the atmosphere rotate about Athe planet in only 4 Earth-days, despite the slow rotation of the @surface. The surface pressure on Venus is about 90 times that on >Earth, and the temperature is 500 degrees Celsius (900 degrees <Fahrenheit). This high temperature is due to the "greenhouse >effect": short-wavelength (visible) light is able to penetrate @the thick atmosphere, but longer-wavelength radiation emitted by ?the warmed planet is absorbed by the blanket of carbon dioxide. @This causes the temperature to increase until the amount of heat ?that can "leak" from the planet comes into equalibrium with the solar energy received. 8 Spacecraft, and Earth-based radrs can penetrate the @enshrouding cloads to reveal surface features. Radar images show <wide volcanic plains that surround regions of maredly higher ;elevation. The largest highland areas, Aphrodite and Ishtar ATerras, are similar in size to earthly continents like Africa and >the Americas. But they seem to have formed in a much different @manner. Earth's crust is made up of distinct, rigid plates that, ?over the aeons, drift across its surface. Venus' crust does not @seem to be broken into rigid plates, but instead moves and takes =form in a more plastic manner. This is a profound difference, ?since Earth's crustal plates determine its large-scale geologic +forms, such as continents and ocean basins. 9 With a crust widely disrupted and marked by abundant Bvolvanism, Venus' surface features appear more diverse than on any @other extraterrestrial body. With its radar capable of producing Ghighly detailed images, the Magellan spacecraft reveals an array of Cvolcanic features and flows, including the longest channel known in ?our solar system. Some features -- given descriptive names like coronae arachnoids tessera (tiles), farrum (pancake-shaped Fdomes), ticks and festoon lavas -- have not been seen on other worlds. < The ages of planetary surface are usually determined by Acounting the craters that have survived resurfacing processes and Cerosion. Erosion on Venus is minimal; without liquid water, surface Cfeatures are worn down mainly by the wind. Yet there are relatively Cfew impact craters, indicating that its geologically active surface <has been renewed throughout much of its history. -- Robert APapalardo, Planetary Geology Group, Arizona State University, and 'Ellen Stofan, Jet Propulsion Laboratory Mass: 0.815 Earth-mass Number of Satellites: 0 Diameter: 12,100 km Length of Day: 243 Earth-days !Length of Year: 0.615 Earth-years Mean Orbital Velocity: 35 km/sec !Mean Distance From Sun: 108 E6 km Venus-Page EARTH E Earth, the planet of blue water, is our home. Alone in the solar Dsystem, it is the home of a robust living skin called the biosphere. DLiving things have been on Earth for at least 3.5 of the 4.5 billion Fyears of the planet's history, and this life has profoundly influenced ,the chemistry, geology and climate of Earth. F Our planet's great beauty and color came into sharp focus with the Bfirst viewing of Earth from space in the late 1960s. This shift in Eperception has stimulated scientific awareness of the interconnection Bamong the geology, the atmosphere, the great oceans and the living Horganisms that affect and are affected by these physical systems. Truly, Ethe history of Earth without the biosphere would have produced a very *different world from the one we see today. H The presence of free oxygen and the chemical and oxidation state of Hmany other gases in the atmosphere are directly due to the activities of Flife. These substances, in turn, affect the temperature and climate of FEarth through mechanisms like the "greenhouse effect," which may cause >global warming. The ocean's chemistry results from the complex Ginteraction of inorganic geological processes and biological activities +that produce many compounds unique to life. G The vast quantity of liquid water on the planet and the remarkable Gactivity of plate tectonics greatly affected the origin of life and its Bevolution on Earth. The continents move over the planet's surface, Dchanging the currents and climates of the land. This has alternately Eseperated and brought together countless different kinds of organisms Hunder myriad conditions. Indeed, the combination of all these properties ;may have been requisite for the diversity of life on Earth. E We are only just beginning to catch a tantalizing glimpse of the Dcomplex choreography of life on a planet. We are on the threshold of Hmajor leaps in understanding of the workings of our home planet. This is Ha very exciting time to be an inhabitant of the lovely planet, Earth. -- Penelope J. Boston, National Research Council Associate, NASA/Langley Research Center Mass: 1 Earth-mass Number of Satellites: 1 Diameter: 12,756 km Length of Day: 1 Earth-day "Length of Year: 365.256 Earth-days #Mean Orbital Velocity: 29.79 km/sec #Mean Distance From Sun: 149.6 E6 km Earth-Page G Mars is more like Earth than any other object in our solar system, Galthough its only half as large. It has mountains and valleys, volcanos Cand earthquake faults, dry river beds and polar ice caps. It has an Gatmosphere with clouds, winds and dust storms. It has summer and winter Dseasons. Its surface is solid and composed mainly of silicon dioxide F(sand). And its temperature is moderate by astronomical, if not human, Estandards. Consequently, it is the only place beyond the Moon that we can seriously consider visiting. D The contrasts are more striking than the similarities, however. HBecause its crust is very thick and rigid, there is no continental drift Eon Mars and no mountain ranges like the Sierras or the Himalayas. But Evolcanos erupting over billions of years have built up mountains that Hdwarf any on Earth. Its polar caps are composed mainly of carbon dioxide Eice, but the northern cap evaporates in the summer, leaving a smaller cap containing only water ice. E The atmosphere is about 95 percent carbon dioxide, with nitrogen Cand argon next in abundance. Its pressure and density are about 100 Etimes less than on Earth, and they fluctuate by about 30 percent with Dthe seasonal waxing and waning of the polar caps. Mars receives less Fthan half the intensity of sunlight as Earth and, primarily because of Cits meager and transparent atmosphere, its is a very cold place. In Fsummer the air temperature never gets up to the melting point of water Aice, and in winter it often falls to the freezing point of carbon Fdioxide, -180 degrees Fahrenheit. Being so cold, the atmosphere cannot Hhold much water vapor, even though the lower levels are often saturated. FAs it never rains, the presence of many dry river beds, both large and -small, is one of the major mysteries of Mars. C The composition of the soil is about one-fifth ferric oxide -- Frusty iron -- which accounts for the red color of both the surface and the sky. E For scientists in many fields, Mars is a fascinating laboratory. EMeteorologists are interested in the modes of atmospheric circulation Gthat don't occur on Earth. Geologists are interested in the composition Gand structure of the interior, the way surface features have formed and Fare still evolving. Biologists are interested in whether any primitive Elife-forms ever existed, and it not, why not. Some of these questions Emay be solved by remotely controlled spacecraft in the next decade or Ctwo, but others will have to wait for people to walk on the surface Ksometime in the next century. -- Conway Snyder, Jet Propulsion Laboratory Mass: 0.1074 Earth-mass Number of Satellites: 2 Diameter: 6,786 km Length of Day: 1.02 Earth-days !Length of Year: 1.881 Earth-years #Mean Orbital Velocity: 24.13 km/sec #Mean Distance From Sun: 227.9 E6 km Mars-Page JUPITER G Jupiter is aptly named for the king of the gods in the Greco-Roman Fpantheon. This planet is more massive than all of the others combined, Cplus their satellites, the asteroids and all comets. Jupiter has 16 Fknown satellites, and the largest, Ganymede, is bigger than the planet EMercury. The planet's magnetic field is so powerful that it creates a Esphere of influence around Jupiter that is larger than the Sun. As if Hall this were not enough, the Voyager spacecraft discovered that the Eplanet has a tenuous ring system and that its Moon-sized satellite is Iwracked by volcanism far more intense than any we find on our own planet. D Even in a small telescope, Jupiter is distinguished by bands of Cclouds that change their appearance over time. More remarkable is a Fpersistent pattern of winds that have lasted for the many decades that Ethe planet has been observed from Earth. The huge oval storm known as 8the Great Red Spot has persisted for at least 300 years. F Jupiter's atmosphere is composed primarily of hydrogen and helium Fin nearly the same abundances that we find in the Sun and other stars. hThe expected hydrogen-dominated compounds methane (CH ), water (H O) and Tammonia (NH ) have all been found, but we've also seen unanticipated fcompounds, acetylene (C ), carbon monoxide (CO) and hydrogen cyanide D(HCN), for example. These substances are formed by ultraviolet light Efrom the Sun, lightning discharges within the clouds and the internal heat escaping from the planet. E The composition of the clouds is still a mystery. The white ones Care almost certainly ammonia cirrus, but a variety of pale pastels, Dmainly variations in yellow and brown with some salmon and blue-gray @patches, indicates that chemical reactions are producing colored Csubstances from the main gaseous constituents. Sulfur compounds are Flikely sources of such colors, but no firm identification has yet been made. H Jupiter's deep gaseous atmosphere merges imperceptibly into a layer Eof liquid hydrogen. Within the planet pressure and temperature are so Ghigh that there is no clear boundary between the gas and liquid. Closer @to Jupiter's center, the pressure becomes high enough to squeeze Celectrons out of hydrogen atoms so they can move freely through the Gliquified gas as they do in metals. Jupiter's intense magnetic field is Cgenerated within this highly conducting layed of metallic hydrogen. G The wealth of phenomena on display at Jupiter invites us to return ?again to learn more about the fundamental physical and chemical Gprocesses that have produced the planets and shaped their environments. Tobias Owen, State University of New York at Stony Brook Mass: 317.89 Earth-masses Number of Satellites: 16 Diameter: 142,796 km Length of Day: 0.41 Earth-day !Length of Year: 11.86 Earth-years #Mean Orbital Velocity: 13.06 km/sec #Mean Distance From Sun: 778.3 E6 km Jupitor-Page SATURN B Ever since 1610 when Galileo first looked at Saturn through a Btelescope, the planet has been distinguished by its prominent ring Bsystem. Now that we have traveled to Saturn with our spacecraft we @realize the full significance of this miniture planetary system. H Saturn is one of the gas giants in our solar system. It's comprised Emainly of hydrogen gas, with a diameter about 10 times that of Earth. GStretching from nearly the outer atmosphere of the planet to the middle Aof the satellite system, the rings are made up of countless small Aparticles ranging in size from dust to mountain-sized masses. The Dthickest part of the ring system, easily seen in photographcs of the @planet, looks like a grooved phonograph record and is made up of Dhundreds of individual features. We now know that these features are Gcaused by the gravitational forces from Saturn's moons orbiting nearby. H The study of these features not only has revealed information about Ethe rings and moons of Saturn, but also about the physics of disks of Amaterial. This knowledge is being applied to other planetary ring Esystems, to the study of the formation of planets around other stars, Fand even to our understanding of the spiral structure of galaxies. The Esaturnian system of planet, moons and rings has provided a laboratory ;for the study of many planetary and astrophysical problems. E Besides these important scientific contributions gained by their ?study, the rings of Saturn are also one of the most awesome and Fbeautiful sights in our solar system. So widespread is the recognition ?of the rings of Saturn that their image has come to represent a Huniversal symbol for "outer space." -- Richard Terrile, Jet Propulsion Laboratory Mass: 95 Earth-masses Number of Satellites: 18 Diameter: 120,000 km Length of Day: 0.43 Earth-day !Length of Year: 29.46 Earth-years "Mean Orbital Velocity: 9.64 km/sec #Mean Distance From Sun: 1,427 E6 km Saturn-Page URANUS F A remarkable thing about Uranus is that its axis is almost in its Borbital plane -- that is, the planet it tilted onto its side. More Eremarkable yet, the orbits of its five moons are titled the same way. FThe magnetic axis does not share this regularity: It is midway between Dthe pole and equator -- the greatest tilt known for any planet. Like FJupiter and Saturn, the surface, if any, is buried at enormous depths; Aall we can see is atmosphere and clouds. The atmosphere is mostly Chydrogen and helium, nuts it's at least 10 times richer in methance ) than those of Juptier and Saturn; Voyager 2 even observed a dense Wmethane cloud layer. If ther are other clouds of ammonia (NH ) or water O), they too are deeply buried. E The spiderey ring system was discovered in 1978 as Uranus passed Fover (occulted) a star, and many occultations have been observed since Bthen. The proposal that individual planetary rings are confined by H"sheperding moons" arose from these results; later this idea was applied Oto detail in the saturnian rings found by the Voyagers Voyager 2 found Ba very extended corona, or outermost atmosphere, of hydrogen atoms Fenveloping the uranian rings. This medium must exert large drag forces Don ring particles and cause them to spiral into the atmosphere, just Hlike a re-entering satellite. Many workers believe that the rings we see Fare temporary, having been formed by collision between unkown moonlets in the last few million years. D Other collisions are evident in the tiny moon Miranda, which was Kunusually well-photographed by Voyager 2 . Its incredibly patchy surface Hmust be the result of the moon's complete breakup into large pieces that Gremained in orbit about Uranus, eventually reassembling into the rubble Apile we see today. The most likely projectile in such an event is Acometary nucleus; such bodies are probably abundant at this great >distance from the Sun. -- D.M. Hunten, University of Arizona Mass: 14.54 Earth-masses Number of Satellites: 15 Diameter: 51,100 km Length of Day: 0.79 Earth-day Length of Year: 84 Earth-years !Mean Orbital Velocity: 6.8 km/sec #Mean Distance From Sun: 2,875 E6 km Uranus-Page NEPTUNE G Neptune is over 50 percent farther from the Sun than its near twin Bin size and appearance, Uranus, but its temperature is equal to or Hslightly greater than that of Uranus. Its internal enery is such that it Femits nearly 2.5 times as much energy as it receives from the Sun. The ?escaping internal energy may also power the storms and winds of ENeptune's atmosphere, which are the fastest in the solar system. Like Cother gas giant planets, Neptune probably has no solid surface. The Fplanets observable atmosphere is primarily hydrogen and helium, and it ?owes its beautiful blue color to an abundance of methane in its Fatmosphere, which absorbs red light and refelects blue. High clouds of Imethane ice cast shadows on deeper, possibly ammonia, ice crystal clouds. H Earth-based observations had hinted at a system of broken rings, or Farcs, around Neptune, but Voyager 2's images revealed a sparse but Gcontinuous ring system. Neptune's outermost ring has three dense areas. HThe next ring in is also narrow but without denser ring arc regions. Two Hbroad inner regions of ring material complete the neptunian ring system. HThe rings are embedded ina magnetic field tilted 50 degrees to Neptune's Eequator and offset from the center of the planet by more than half of its radius. H Voyager 2 added six small moons to Neptune's known retinue, all @relatively close to the planet. Tiny Nereid, the outermost moon, Foccupies the most eccentric orbit of any moon in the solar system. But HTriton is the most curious of Neptune's satellites. It is the only large Jmoon in the solar system to orbit "backwards" around the planet. Voyager found Triton to have a tenuous nitrogen atmosphere, the coldest Bsurface temperatures in the solar system, an enormous polar cap of Hnitrogen ice and active geyser-like plumes erupting through the ice cap. GTriton may well be a Pluto-like object, formed independently of Neptune Fin the outer solar system but later "captured" by the planet's gravity E.D. Miner, Jet Propulsion Laboratory Mass: 17.15 Earth-masses Number of Satellites: 8 Diameter: 49,500 km Length of Day: 0.67 Earth-day !Length of Year: 164.8 Earth-years !Mean Orbital Velocity: 5.4 km/sec #Mean Distance From Sun: 4,500 E6 km Neptune-Page PLUTO H Discovered in 1930 by Clyde Tombaugh from the Lowell Observatory in GFlagstaff, Arizona, Pluto is the most recently discovered planet. It is Fthe only planet that will not be visited by spacecraft during the 20th Acentury and so, for some time to come, Pluto will remain the most Genigmatic planet. Because Pluto is smaller than Earth's Moon and orbits Gat a tremendous distance from the Sun, it is only a bright speck in the strongest telescopes. F Unlike the other planets that orbit beyond Mars -- the gas giants G-- Pluto is small, with only a very thin atmosphere, composed mainly of Rmethane ( CH ) gase, and orbits the Sun in a steeply inclined and Geccentric orbit. For about 20 Earth-years out of each 248.5 year orbit, BPluto is actually closer to the Sun than is Neptune. Pluto will be Btraversing this part of its orbit between 1980 and 1999. It passed 7perihelion ( its closest approach to the Sun ) in 1989. @ Pluto is practically a double planet. Its satellite, Charon G( discovered in 1978 by James Christy of the US Naval Observatory ), is Hthe largest satellite relative to its parent planet in the solar system. GCharon's diameter of some 1,200 kilometers is about half that of Pluto, Fand it orbits its planet at a distance of 17 Pluto radii. In contrast, Gour Moon's diameter is about one-quarter of Earth's, which it orbits at Fa distance of about 60 Earth radii. Like Pluto, Charon may also have a @thin atmosphere, but we have not yet determined its composition. H Charon's orbital period is equal to Pluto's rotation period, so the Flength of a plutonic day and month are the same. Because of this, to a Bperson standing on Pluto directly under Charon the satellite would Happear to remain stationary, forever hanging over that spot. Conversely, Ha person on the diametrically opposite side of Pluto would never see the satellite at all! F Pluto's surface is covered with a methance ice, while Charon's is Hcovered with water ice. This strange pair, locked in distant orbit, will Gbe an extremely intriguing target for exploratory spacecraft in what we Ehope will be the not-too-distance future. -- Edward F. Tedesco, Jet Propulsion Laboratory Mass: 0.0022 Earth-mass Number of Satellites: 1 Diameter: 2,300 km Length of Day: 6.4 Earth-days !Length of Year: 248.5 Earth-years !Mean Orbital Velocity: 4.7 km/sec #Mean Distance From Sun: 5,900 E6 km Pluto-Page SolarSystem-Form SolarChart Mercury_Button Earth-Button Jupiter_Button Mars_Button Uranus_Button Venus_Button Neptune_Button Saturn_Button Pluto_Button ABOUT Solar-Page J FORM ILBMBMHD '0xp0 ' xp0 y>2s3 y>0s3 rfr2s3 rfr2s3 rfrBs rfrBs rNrrs rNrrs rfrrs ~rfrrs ILBMBMHD <<<UUUdddttt 7iKRs ^,21P _\!fg +v/pEp 9|ILBMBMHD <<<UUUdddttt `&M?? 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Founded in 1980, the Society now has Fmore than 100,000 dues-paying members in the United States, Canada and Cover 50 other nations. Members receive the colorful and informative @magazine, The Planetary Report , discounts on books and other <educational materials, and the opportunity to participate in @Society-sponsored activies. For more information, write or call: The Planetary Society 65 N. Catalina Avenue Pasadena, CA 91106 818-793-5100 AUTHOR ,ABCUG User Group Wishbringer BBS *PO Box 179 410-269-6607 Glen Burnie, MD 21060 =Internet: korczyns@oasys.dt.navy.mil or joekjr@cup.portal.com AUTHOR /ABCUG User Group Wishbringer BBS ,PO Box 179 410-269-6607 Glen Burnie, MD 21060 ?Internet: korczyns@oasys.dt.navy.mil or joekjr@cup.portal.com ABOUT THIS BOOK MThis book was created with information provided by The Planetary Society The Planetary Society is a non-profit, tax-exempt membership organization Cdedicated to the exploration of the solar system and the search for Eextraterrestrial life. Founded in 1980, the Society now has more than D100,000 dues-paying members in the United States, Canada and over 50 Eother nations. Members receive the colorful and informative magazine, The Planetary Report , discounts on books and other educational materials, Aand the opportunity to participate in Society-sponsored activies. $For more information, write or call: The Planetary Society 65 N. Catalina Avenue Pasadena, CA 91106 818-793-5100 Info-Page About The Author #Click To Return To Our Solar System