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Spitzer Constraints on Primordial and Debris Disk Evolution

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)

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Spitzer Constraints on Primordial and Debris Disk Evolution

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  1. 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) M. Meyer (Arizona) A. Moro-Martin (Princeton) P. Morris (SSC) J. Najita (NOAO) D. Padgett (SSC) I. Pascucci (Arizona) J. Rodmann (MPIA) M. Silverstone (Arizona) D. Soderblom (STScI) J. Stauffer (SSC) B. Stobie (Arizona) S. Strom (NOAO) D. Watson (Rochester) S. Weidenschilling (PSI) S. Wolf (MPIA) E. Young (Arizona) Spitzer Constraints on Primordial and Debris Disk Evolution John Carpenter on behalf of the FEPS collaboration

  2. Parameter Space for FEPS and Upper Sco 20 Upper Sco (205 stars) FEPS (314 + stars) Stellar Mass (Msun) 1 0.1 3 5 3000 Stellar Age (Myr)

  3. Disks vs. Stellar Mass at 5 Myr StellarMass Excess

  4. FEPS: 8m excesses Excess < 1.3% excess (3) for < 100 Myr See also Silverstone et al. (2006)

  5. FEPS: 24m excesses 3 = 12%

  6. 24m Excess Fraction vs. Age

  7. 70m Excess Fraction vs. Age

  8. Dust temperatures

  9. IRS Dust Temperature vs. Age

  10. Debris Disk Models Terrestrial Planet Formation Kuiper Belt disks Kenyon & Bromley (2005)

  11. Evolution of Hot Dust Dominic & Decin (2003) Wyatt et al. (2007) FEPS 8m limit (3)

  12. Evolution of Warm Dust

  13. Evolution of Cool Dust

  14. Gas Dissipation Timescales H2 H2 S I Fe II H2 Si II Pascucci et al. 2006

  15. Gas Dissipation Timescales < 0.04 MJup in inner disk for ages 10-100 Myr < 2 Mearth between radius of 10 and 40 AU Pascucci et al. 2006

  16. Summary • Primordial 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

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