spitzer constraints on primordial and debris disk evolution
DESCRIPTION
D. Backman (NASA-Ames) S. Beckwith (STScI) J. Bouwman (MPIA) M. Cohen (UC-Berkeley) U. Gorti (NASA-Ames) T. Henning (MPIA) L. Hillenbrand (Caltech) D. Hines (Space Sci. Inst) D. Hollenbach (NASA-Ames) J. Kim (Arizona) J. Lunine (LPL) R. Malhotra (LPL) E. Mamajek (CfA) - PowerPoint PPT PresentationTRANSCRIPT
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Spitzer Constraints on Primordial and Debris Disk EvolutionJohn Carpenter on behalf of the FEPS collaboration
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Parameter Space for FEPS and Upper ScoStellar Age (Myr)5330000.1201Stellar Mass (Msun)FEPS (314 + stars)Upper Sco (205 stars)
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Disks vs. Stellar Mass at 5 Myr
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FEPS: 8m excesses< 1.3% excess (3) for < 100 MyrSee also Silverstone et al. (2006)
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FEPS: 24m excesses3 = 12%
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24m Excess Fraction vs. Age
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70m Excess Fraction vs. Age
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Dust temperatures
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IRS Dust Temperature vs. Age
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Debris Disk ModelsKenyon & Bromley (2005)Terrestrial Planet FormationKuiper Belt disks
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Evolution of Hot DustFEPS 8m limit (3)Dominic & Decin (2003)Wyatt et al. (2007)
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Evolution of Warm Dust
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Evolution of Cool Dust
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Gas Dissipation TimescalesPascucci et al. 2006H2H2S IH2Si IIFe II
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Gas Dissipation TimescalesPascucci et al. 2006< 0.04 MJup in inner disk for ages 10-100 Myr< 2 Mearth between radius of 10 and 40 AU
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SummaryPrimordial disks survive longer around low mass stars
12% solar mass stars with > 12% excess at 24 m for < 300 Myr
Decline in 24 m excess fraction > 300 Myr
Uranus/Neptune-mass planets form by 100 Myr