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class21a - AST 309S The Solar System MWF 11-12 John Lacy...

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AST 309S The Solar System MWF 11-12 John Lacy RLM 16.332, M-F 12-12:30 471-1469 [email protected] Amanda Bayless Daniel Kagan RLM 16.312, Th 10-12 RLM 16.322A, W 3-5 471-3462 471-6858 [email protected] [email protected] class website: www.as.utexas.edu courses AST 309S username: AST password: 309
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Topics from chapter 5.5-5.7 Goldilocks evaporation and condensation of water, vapor pressure atmospheric motion, Hadley cells troposphere stratosphere, ozone layer thermosphere and ionosphere magnetosphere
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Reading for this week Chapter 5: Atmospheres of Terrestrial Planets Today Convection and Wind (We’re not covering everything in the chapter. There will be one question on the test on a topic in the book, that wasn’t in the lectures, but is on the list of review topics.)
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Origin of the terrestrial atmospheres When the terrestrial planets formed, they were hot enough that most common gasses had escape speed, so they formed without atmospheres. The atmospheres came from molecules that were in the rocks that formed the interiors of the planets. When these rocks were heated inside of the planets, gasses were released.
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CO 2 Carbon was in the form of graphite and carbonate minerals when the terrestrial planets were formed. Carbon in graphite could combine with oxygen to make CO 2 , and when carbonate minerals (limestone) are cooked inside of planets they can release CO 2 . The main way CO 2 can be removed from an atmosphere is by being dissolved in water and forming limestone. On the Earth, CO 2 is also removed from the atmosphere by plants, which convert it and H 2 O to cellulose and O 2 . And it is returned to the atmosphere when those plants decay (perhaps inside of animals) or are burned (perhaps after being converted to coal or oil).
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H 2 O There never was liquid water on Venus. It’s too hot.
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