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Cratered Worlds: The Moon & Chapter 7 Mercury The Moon • Mass 1/80 of Earth’s mass • Gravity 1/6 of Earth’s • Atmosphere – no real atmosphere – few volatiles (elements that evaporate at relatively low temperatures; e.g. water) Apollo 17 Dec 1972 Lunar Surface • Dominant Features – Craters – Maria = “seas” • Dark features • Radioactive dating (moon rocks) – age 3.3 - 4.4 billion yrs – older than rocks on Earth • Earth-Moon system about 4.5 billion years old Geological Features • Surface dominated by impacts • Highlands – heavily cratered, light colored • oldest parts of surface – silicate rocks • Maria – 17% of surface, mostly on near side – dark material, fewer craters • youngest parts of surface – volcanic plains of basalt • lava-filled impact basins Composition & Structure • Average density – 3.3 g/cm3 • lower than Earth’s mantle (5.5 g/ cm3) • Similar to Earth’s crust QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. • Composition – mostly lighter silicates – depleted in iron – similar to Earth’s crust • Mantle – solid – little seismic activity Not geologically active (now) • Core – Small, possibly iron rich – solid and cold Differentiation Moon’s interior molten in past Impact Craters • Not erased by erosion (no atmosphere) – preserved record of impacts – indicator of solar system history • Crater Origin – not volcanic – meteor impacts • surface “explosions” • creates circular craters – typical characteristics • bowl-shaped • turned up rims • central peaks Crater Counts • Number of craters indicates age – many craters = old – few craters = young • Ongoing impacts – during last 3.8 billion yrs • Compare: highlands vs. maria – maria formed 3.8 billion years ago • Based on number of craters – highlands have many more craters • highlands older • Conclude: – Period of heavy bombardment • prior to 3.8 billion years ago A moon covered with numerous and very old craters created by meteorite impacts likely a) b) c) d) has no ocean to cover the craters. orbits a large Jupiter sized planet. has a cold, solid interior. has no protective magnetic field. Formation of Moon QuickTime™ and a GIF decompressor are needed to see this picture. Giant Impact Theory .erut cip sih t ee s ot ded een era ro s serp moc ed )d e s ser p mo cn U( FF IT a dna ™e mi Tk ciuQ Mercury • Closest planet to sun • Surface similar to Moon – heavily cratered – no atmosphere • Only one spacecraft flyby – Mariner 10 flew by 3 times in 1974-75 – New mission Messenger is in planning stages Mercury - Structure • Second smallest of planets by mass and size – Mass 1/18 of Earth’s mass – Radius less than half of Earth’s – Pluto is only planet smaller • Density 5.4 g/cm3 – denser than Earth’s mantle – quite different from Moon • Dense iron-nickel core – 60% of total mass – almost size of Moon! Quic k Ti me™ and a T IFF (Unc om pres s ed) dec om pres s or are needed to s ee t his pic t ure. Mercury - Surface • No evidence of tectonic activity • Scarps (cliffs) in middle of craters – crust shrank and cracked (after craters formed) Quic kTime™ and a TIFF (Uncompress ed) dec ompres sor are needed to see this pic ture. Earth-Like Planets: Venus and Mars QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Chapter 7 View from Earth • Venus shows phases – otherwise featureless Quic kTime™ and a TIFF (Uncompress ed) dec ompres sor are needed to se • Obscured by clouds • Mars appears red – due to iron oxides (rust) – polar ice caps – surface markings • Seasonal changes Quick Time™a nd a TIFF ( Uncomp res sed) dec ompr esso r ar e need ed to see this pictur e. Martian Canals QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. • Schiaparelli (1877) reported canale on Mars – Italian = “channels” – English = “canals” • Led to suggestion of intelligent Martian civilization – War of the Worlds (H.G. Wells) • Percival Lowell primary American proponent • Eventually shown to be optical illusion QuickT ime ™an d a TIFF (Un compr ess ed) d ecomp res sor a re ne eded to se e th is p ic tu re. Highlights • Venus: – seems a “twin” of Earth (but not!) – massive atmosphere • large greenhouse effect • surface temp about 750 K • Mars: – quite cold • once much warmer – very thin atmosphere • once much thicker – had flowing water in past • possibility of life? Venus: General Properties • Mass – 82% of Earth’s mass • Radius – about same as Earth • Density (5.3 g/cm3) – about same as Earth Surface of Venus • Problem: how to see through cloud cover? • Spacecraft exploration – Venera 7 (USSR) • landed on surface (1970) • lasted 23 minutes! – Magellan Orbiter (USA) • use radar imaging (from orbit) • mapped surface at 100m resolution Radar Map of Venus Surface of Venus • Surface features – produced by volcanic and tectonic activity – but no plate motion – 75% low lava plains • produced like lunar maria • very “young” surface (few craters) – 25% mountains/mountain ranges Craters on Venus • Few small craters – small objects burn up in dense atmosphere • Use large (>30 km) craters to estimate age – lava plains 500-600 million yrs • vast geologic activity then • not much since QuickTi me™ and a TIFF (U ncompressed) decompressor are needed to see this picture. Atmospheric Conditions • Extreme atmospheric pressure / density – 100x greater than Earth • Very high surface temps – around 750 K – little day/night variation • due to thick atmosphere • Generally hot and dry – no water • Occasional “acid rain” – sulfuric acid clouds Atmosphere of Venus • Layers of sulfuric acid clouds – 30-60 km above surface • Composition – 96% carbon dioxide – 3% nitrogen – remove CO2, then atmos. like Earth’s • Runaway greenhouse effect – – – – Greenhouse gasses -> high temps water evaporates carbon dioxide CO2 released from rocks increases greenhouse Mars: General Properties • radius – about 1/2 of Earth’s • density 3.9 g/cm3 – less than Earth; more than Moon – mostly silicates – possible metal core Qu i ck Ti me ™a nd a TIFF (Unc om pres se d) de co mp re ss or are n ee de d to s ee th is pi ctu re . • Rotation – period 24 hours, 37 min (like Earth) • tilt of axis about 25º; orbital period 1.88 years – seasons similar to Earth’s – duration ~ 6 months (instead of 3) Surface Conditions • Temperatures – Summer: • • • • Day 240 K (-33 C) Night 190 K (-83 C) Coldest 173 K (-100 C) Water frost deposits • Surface winds mostly moderate – but giant dust storms can occur QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. MGS Images of Opportunity Landing Site QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. MGS Images of Opportunity Landing Site QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Mars Atmosphere & Climate • Composition: – 95% carbon dioxide (CO2) – 3% nitrogen (N2) – similar to Venus! • Atmospheric pressure – 100x smaller than Earth’s QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture – equiv. to 30 km above Earth surf. • Clouds – dust clouds – water ice clouds – dry ice (CO2) crystals Polar Caps • At both N and S poles – change with seasons – seasonal ice caps • composed of dry ice (frozen CO2) – permanent ice caps • composed of water ice QuickTime™ and a TIFF (Uncomp resse d) de com press or are nee ded to s ee this picture. Seasonal Changes QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Channels and Flood Plains • Evidence liquid water existed on Mars – highlands runoff channels • from ancient rainstorms? • older than 3.9 million yrs – outflow channels • much larger • carved by huge floods QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Climate Change • Evidence indicates – Mars had liquid water (warmer) – much denser atmosphere • What happened? • “Runaway refrigerator effect” – atmosphere began to escape into space (low gravity) • • • • • less dense atmosphere -> less greenhouse surface cools water freezes -> less greenhouse more cooling carbon dioxide freezes -> less greenhouse – happened over 3 billion yrs ago Planetary Evolution • Earth, Venus, & Mars: – very different results from planetary evolution – why so different when they started similarly? • Runaway greenhouse (Venus) • Runaway refrigerator (Mars) • Could Earth change drastically? – what triggered changes? • Could Mars be made habitable? – terraforming