class12a - AST 309S The Solar System MWF 11-12 John Lacy R...

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AST 309S The Solar System MWF 11-12 John Lacy RLM 16.332, M-F 12-12:30 471-1469 lacy@astro.as.utexas.edu Amanda Bayless Daniel Kagan RLM 16.312, Th 10-12 RLM 16.322A , W 3-5 471-3462 471-6858 baylessa@astro.as.utexas.edu kagan@astro.as.utexas.edu class website: www.as.utexas.edu courses AST 309S username: AST password: 309
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Topics from chapter 4 How can planetary surfaces be modified? impact cratering – especially on Mercury and Moon lava flows – especially on Venus and Earth weathering – especially on Earth and Mars formation of craters dating surfaces from crater counts effects of wind and water resurfacing by extensive lava flows evidence of water on Mars
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Reading for this week Chapter 4: Surface changes I hope we’ll have the test graded by Friday. Today Crater formation and dating of surfaces
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Number of craters Mercury and the Moon are saturated with craters. That is, there are craters pretty much everywhere, with craters on top of craters. But there are many fewer craters on Venus, Earth, and Mars (except in the highlands near Mars’ south pole). Why are there so many fewer craters on Venus, Earth, and
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class12a - AST 309S The Solar System MWF 11-12 John Lacy R...

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