lec20_14nov2011

lec20_14nov2011 - Can we study extrasolar Kuiper Belts Pic...

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Ge/Ay133 Can we study extrasolar Kuiper Belts? β Pic, A5V star AU Mic, M1Ve star
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Impossible to see any exo-KBOs themselves, but…
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How do we find debris disks? Model has 0.1 M moon of 30 μ m size dust grains in a disk from 30–60 AU Bars are 3 σ Model based on disks around A stars Spitzer Data (FEPS team) Meyer et al., ApJS, 154, 422
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What have far-IR SED surveys found?: Overall decay consistent with erosional evolution, fluctuations dominated by large collisions? Rieke et al., ApJ, 620, 1010
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So, when rings are seen around >10 Myr old stars… the dust must be made in place. CSO/HST have reached similar  conclusions about structure of the disk  around Fomalhaut and how it is  generated. Is there a planet required to  maintain it (Kalas et al. 2008)? Marsh et al. – ApJ, Feb. 2005 Kalas, Graham, & Clampin – HST, Nature, June 2005
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Vega arcsec arcsec
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This note was uploaded on 01/03/2012 for the course GEL 133 taught by Professor List during the Fall '10 term at Caltech.

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lec20_14nov2011 - Can we study extrasolar Kuiper Belts Pic...

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