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Gas in Transitional Disks

Gas in Transitional Disks. Sean Brittain Clemson University, Clemson, SC, USA Joan Najita National Optical Astronomy Observatory, Tucson, AZ, USA. 5 th Planet Formation Workshop. Interpretation of the SED. Interpretation of the SED. Malfait et al. 1998. Gas in Transitional Disks.

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Gas in Transitional Disks

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  1. Gas in Transitional Disks Sean Brittain Clemson University, Clemson, SC, USA Joan Najita National Optical Astronomy Observatory, Tucson, AZ, USA 5th Planet Formation Workshop

  2. Interpretation of the SED

  3. Interpretation of the SED Malfait et al. 1998

  4. Gas in Transitional Disks FFv 

  5. Gas in Transitional Disks

  6. 100 AU ~50 K 10 AU ~500 K 0.1 AU ~2000 K Gas in Transitional Disks E”J=2~500K,J1 H2 UV, NIR, MIR H2O ro-vib Freezes at ~170K OH Dv=1 FIR [OI], [CI] CO Dv=1 CO Dv=0 CO Dv=2

  7. Kinematic Information From Spectroscopy

  8. NIR AB Aurigae A0 star “Classic Disk” Age ~ 4 Myr F/vFv . Regions of interest Wavelength (m) C. Grady, et al. 2003, ApJ, 683, 151 NIR HD 141569 A0 star “Transitional Disk” Age ~ 6-8 Myr . F/vFv Wavelength (m) Clampin, et al. 2003, AJ 126, 385 Malfait et. al. A&A 331: 221 (1998)

  9. Using NIR Spectroscopy to probe the inner disk: CO HD 141569 . AB Aur .

  10. T=5600 K Blue: Model (R=9-40AU) Red: Data

  11. HD 100546: A Transitional Disk Grady et al. 2005 See also Acke et al. 2006 and Bouwman et al. 2003

  12. HD 100546 • Rin(dust)~10AU • Rin(CO)=7 AU • Rout(CO)>50 AU

  13. Conclusions • Need data on gas in disk to properly interpret the SED • CO is a robust tracer of warm gas in transitional disks around early HAe and late HBe stars • Non-detection of ro-vibrational CO emission can rule out presence of gas within ~50AU

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