Gas in Transitional Disks

Sean BrittainClemson University, Clemson, SC, USA

Joan NajitaNational Optical Astronomy Observatory, Tucson, AZ,

USA

5th Planet Formation Workshop

Interpretation of the SED

Interpretation of the SED

QuickTime™ and aTIFF (Uncompressed) decompressor

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Malfait et al. 1998

FF

v

Gas in Transitional Disks

Gas in Transitional Disks

Sicilia-Aquilar et al. 2005

Gas in Transitional Disks

0.1 AU~2000 K

10 AU~500 K

100 AU~50 K

H2O ro-vib

CO v=2

CO v=1

H2 UV, NIR, MIR

OH v=1

E”J=2~500K, J1

Freezes at ~170K

CO v=0

FIR [OI], [CI]

Kinematic Information From Spectroscopy

Malfait et. al. A&A 331: 221 (1998)

NIR

NIRA0 star“Transitional Disk”Age ~ 6-8 Myr

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Regions of interest

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A0 star“Classic Disk”Age ~ 4 Myr

Clampin, et al. 2003, AJ 126, 385

C. Grady, et al. 2003, ApJ, 683, 151

F/

vFv

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vFv

Wavelength (m)

Wavelength (m)

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HD 141569

AB Aur

T=5600 K

Blue: Model (R=9-40AU)

Red: Data

HD 100546: A Transitional Disk

Grady et al. 2005

See also Acke et al. 2006 and Bouwman et al. 2003

HD 100546

•Rin(dust)~10AU

•Rin(CO)=7 AU

•Rout(CO)>50 AU

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