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Observational constraints on disk photoevaporation by the central star

Published online by Cambridge University Press:  01 May 2007

Gregory J. Herczeg
Gregory J. Herczeg*
Affiliation:
Caltech MC105-24, 1200 E. California Blvd., Pasadena, CA 9125
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Abstract

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We apply results from FUV and X-ray spectroscopy to evaluate the role of photoevaporation in dispersing the disk around TW Hya. Accretion produces bright EUV emission that may be smothered by the accretion column. Solar-like magnetic activity produces fewer ionizing photons, which may be absorbed by an accretion-powered neutral wind. We estimate a photoevaporation rate of ∼ 5 × 10−11M⊙ yr−1 for the disk around TW Hya. These models can be tested by detecting gas in the ionized disk surface, including emission in the [Ne II] 12.8μm line. Photoevaporation is likely a minor process in disk dispersal during the accretion phase, but could remove ∼ 1 MJ of remnant gas around a solar-mass star after accretion ceases.

Keywords

Stars: planetary systems: protoplanetary disksstars: pre–main-sequenceaccretionstars: coronae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 147 - 154
Copyright
Copyright © International Astronomical Union 2007

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