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The nature of stellar winds in the star-disk interaction

Published online by Cambridge University Press:  01 May 2007

Sean Matt  and
Ralph E. Pudritz
Sean Matt
Affiliation:
Dept. of Astronomy, U. of VirginiaPO Box 400325, Charlottesville, VA 22904-4325, USA email: [email protected]
Ralph E. Pudritz
Affiliation:
Physics and Astronomy Dept., McMaster University, Hamilton, ON, L8S 4M1, Canada email: [email protected]
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Abstract

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Stellar winds may be important for angular momentum transport from accreting T Tauri stars, but the nature of these winds is still not well-constrained. We present some simulation results for hypothetical, hot (∼ 106 K) coronal winds from T Tauri stars, and we calculate the expected emission properties. For the high mass loss rates required to solve the angular momentum problem, we find that the radiative losses will be much greater than can be powered by the accretion process. We place an upper limit to the mass loss rate from accretion-powered coronal winds of ∼ 10−11M yr−1. We conclude that accretion powered stellar winds are still a promising scenario for solving the stellar angular momentum problem, but the winds must be cool (e.g., 104 K) and thus are not driven by thermal pressure.

Keywords

MHDstars: coronaestars: magnetic fieldsstars: pre–main-sequencestars: rotationstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 299 - 306
Copyright
Copyright © International Astronomical Union 2007

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