Evolution of Lunar Surface. Lunar Erosion Surface of Mercury.

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Presentation transcript:

Evolution of Lunar Surface

Lunar Erosion

Surface of Mercury

Caloris Impact

Tectonics on Mercury

Surface of Mars

Olympus Mons

Valles Marineris

Ancient Water on Mars

Past Liquid Water

Martian Oceans and Lakes

Ancient Martin Floodplain

Surface of Venus

Volcanoes on Venus

Tectonics on Venus

Pictures from Venus

Geological History

Gases in Atmospheres Volatiles in Molecular Form (ice or gas): –Carbon dioxide CO 2 (molecular weight = 44) –Oxygen O 2 (molecular weight = 32) –Nitrogen N 2 (molecular weight = 28) –Water H 2 O (molecular weight = 18) Other gases: –Argon Ar (molecular weight = 40) –Neon Ne (molecular weight = 20) Jovian gases: –Ammonia NH 3 (17), Methane CH 4 (16), Helium He (4), and Hydrogen H 2 (2)

Understanding Pressure

Surface Temperatures Distance from Sun: the energy received from the Sun is inversely proportional to the square of the distance Albedo: the fraction of reflected sunlight. The darker the surface, the more light energy it absorbs. Rotation Rate Greenhouse Effect

Temperature without Atmospheres

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