Observational constraints on disk photoevaporation by the central star

Details Observational constraints on disk photoevaporation by the central star Observational constraints on disk photoevaporation by the central star

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..243..147h&link_type=abstract

Star-Disk Interaction in Young Stars, Proceedings of the International Astronomical Union, IAU Symposium, Volume 243, p. 147-154

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3

Stars: Planetary Systems: Protoplanetary Disks, Stars: Pre–Main-Sequence, Accretion, Stars: Coronae

Scientific paper

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 × 10-11 M 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.

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