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Ast1141Lec19TerrestrialPlanets.pptx - Terrestrial Worlds in...

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Terrestrial Worlds in ComparisonAstronomy 1141
The Terrestrial PlanetsLarge Bodies:Earth (1 RE, 1 ME)Venus (0.95 RE, 0.82 ME)Small Bodies:Mars (0.53 RE, 0.11 ME)Mercury (0.38 RE, 0.055 ME)Moon (0.27 RE, 0.012 ME)
Impact crateringis only importantduring the first billion years of thesolar system.Volcanism&Tectonicsare driven by theinternal structure of the planets.Is a planet’s interiorhotenough fortectonicsor volcanism?The evolution of planetary surfaces is driven byimpactcratering,volcanism, andtectonics.
Lava plains (Maria) on the MoonLava plains and volcanic vents on MercuryHot-spot volcanoes on MarsCrustal Shaping:Primary crust: shaped byimpactsSecondary crust: shaped byvolcanismMars, Mercury & the Moon:Old, heavily cratered surfaces >3 Gyr oldSingle, continuous crust (no plates)Vertical Tectonism (stationary upwelling)The surfaces of the small terrestrial planets wereshaped primarily by impacts and early volcanism.
Volcanic vents on Mercury[MESSENGER]Hot Spot Shield Volcanoeson Mars[NASA MGS]Evidence of past volcanism on Mercury and Mars
Earth: plate tectonics &lateral recycling:Subduction, sea-floor spreading &up-thrust constantly recycle the crust.Venus: lacks plate tectonics! The reasonis poorly understood.Earth’s surface is ~100 MyroldVenus’ surface is ~500Myr oldThe surfaces of the large terrestrial planets areyoung, with activetertiary crusts.
Pancake DomesMagma upwellingpushes up the crustCoronaeMagma down-wellingcollapsing the crustVery Different GeologyOn Venus

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