Terrestrial_Planets_-3_25feb08

Terrestrial_Planets_-3_25feb08 - Planetary Atmosphere Basic...

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1 Planetary Atmosphere Basic Properties Black Body Radiation Sources of Atmosphere Atmospheric Loss by Thermal Escape Atmospheric Photochemistry Loss of Atmosphere Atmopsheric Evolution – Tools for Tracking Cases: Earth, Mars, Venus and Airless Planets
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2 Basic Properties Pressure = Weight of gas column above Weight of overlying gas decreases as move up vertically therefore pressure decreases. P = P(o) exp ( -z/H) H = Scale Height, P(O) = Pressure at the base. H = ~ 10km for Earth Sunlight warms the planetary surface and the atmopshere. Over time the planets achieve a steady state. Heat from lower levels can make it to the top of the atmosphere and escape in two ways. Radiation and Convection
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4 Loss of Heat However atmosphere may not be transparent to all wavelengths. The escaping heat energy (reflected back) is typically of longer wavelengths. In this case heat loss is impeded, energy is trapped and temperature rises up. This way the temperature of the atmosphere can rise and this is
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This note was uploaded on 09/18/2010 for the course GLG 130 taught by Professor Srinivasan during the Spring '07 term at University of Toronto.

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Terrestrial_Planets_-3_25feb08 - Planetary Atmosphere Basic...

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