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Unformatted text preview: make the math go faster for you! 2. Derive equation 2.3 on page 36, starting with the definition of the orbital velocity for circular orbits. (Hint: this is not a very elaborate derivation, should only be a few lines, and we sort of did it in class.) 3. Refer to the discussion about vertical structure (Chap. 2 section 2). Desch (2007) derived a new equation for the surface density of a disk, " ( r ) = 343 r 10AU # $ % & ’ ( ) 2.168 g * cm2 . Can this disk’s selfgravity still be neglected at 1 AU? 5 AU? 10 AU? Does the approximation (to neglect the disk’s selfgravity) get better or worse as you go further away from the star? Assume a 1 M sun star....
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This note was uploaded on 09/08/2010 for the course ASTR 155 at San Jose State University .
 '10
 Kress,Monika
 Astronomy

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