Interiors of Terrestrial PlanetsMercuryThe Resonant Rotation of MercuryVenusThe External Appearance of VenusRadar Maps of VenusCraters on VenusVolcanoes on VenusThe Real Surface of VenusMarsClouds, Polar Caps, and Odd MarkingsValles Marineris CanyonThe Volcanoes of MarsMartian TerrainsEvidence of Water FlowsThe Surface Desert of MarsThe Martian MeteoriteMartian Moons: Phobos and DeimosThe Atmospheres of the Terrestrial PlanetsThe Greenhouse EffectEvolution of Terrestrial AtmospheresSummary of the Terrestrial PlanetsInteriors of Terrestrial PlanetsMercury •MEAN RADIUS: 2439.7 km •MASS: 0.055 (Earth=1) •DENSITY: 5.43 (g/cm^3) •GRAVITY: 0.376 (Earth=1) •ORBIT PERIOD: 87.97 (Earth days) •ROTATION PERIOD: 58.65 (Earth days) •SEMIMAJOR AXIS OF ORBIT: 0.387 au •ECCENTRICITY OF ORBIT: 0.206The Resonant Rotation of MercuryMercury’s large core may indicate a “mantle-stripping” impact with a similar body.1 solar day =176 Earth days1 sidereal day=59 Earth daysVenus•MEAN RADIUS: 6051.9 km •MASS: 0.814 (Earth=1) •DENSITY: 5.24 (g/cm^3) •GRAVITY: 0.903 (Earth=1) •ORBIT PERIOD: 224.7 (Earth days) •ROTATION PERIOD: 243.0 R (Earth days) •SEMIMAJOR AXIS OF ORBIT: 0.723 au •ECCENTRICITY OF ORBIT: 0.007The External Appearance of VenusVenus in visible light – cloud shroudedVenus in the ultraviolet – cloud patterns rotate every 4 days.Radar Maps of VenusThe Magellan probe provided a high resolution elevation map of Venus, with information on reflectivities that indicate textures.Craters on VenusVolcanoes on VenusThe Real Surface of VenusActual pictures from the ground -- the Soviet Venera seriesTemperature: 800 degrees, Pressure: 100 atmospheresMars•MEAN RADIUS: 3388.0 km •MASS: 0.108 (Earth=1) •DENSITY: 3.94 (g/cm^3) •GRAVITY: 0.380 (Earth=1) •ORBIT PERIOD: 686.98 (Earth days) •ROTATION PERIOD: 1.026 (Earth days) •SEMIMAJOR AXIS OF ORBIT: 1.524 au •ECCENTRICITY OF ORBIT: 0.093Clouds, Polar Caps, and Odd MarkingsMars presents many different aspects to us. Its weather and terrain are varied and changeable.Valles Marineris CanyonThe Volcanoes of MarsMartian TerrainsDune FieldsOld cratered highlandsPolar Ice fieldsEvidence of Water FlowsWater cannot be a liquid on Mars’ surface now, but billions of years ago it flowed (there may even have been seas.The Surface Desert of MarsMars looks like a desert with about the same land area as the Earth. Its pink skies, however, contain far too little pressure to allow outside living.The Martian MeteoriteThis rock IS from Mars.Does it contains signs of life?Stay tuned….Martian Moons: Phobos and DeimosMars’ moons are very small; almost certainly captured asteroids. Phobos orbits in less than a day – retrograde.The Atmospheres of the Terrestrial PlanetsThe Greenhouse Effect1) In equilibrium, a planet must re-radiate all the energy it absorbs.2) Solar energy tends to be converted from visible to infrared radiation.3) Some gases are transparent to visible radiation, but opaque to infrared radiation.4) When radiation is blocked, you need a bigger temperature gradient to push the energy through.Evolution of Terrestrial AtmospheresAll the terrestrial planets start off with a substantial atmosphere. Mars lost most of it because of low escape speed. Earth converted most of the carbon dioxide into rocks. Life produced free oxygen. Venus lost the water because it stayed vapor (and solar UV released hydrogen).Summary of the Terrestrial PlanetsThese are the “rocky” worlds of our inner solar system. The other large solid bodies in the solar system are all moons of the outer gas giant planets. They were collected by impacts of smaller bodies, and still bear those scars and
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