The Nature of Stellar Winds in the Star-Disk Interaction
arXiv:0707.0306 · doi:10.1017/S1743921307009659
Abstract
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 (~1e6 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 ~1e-11 solar masses per year. 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 (~1e4 K) and thus are not driven by thermal pressure.
arXiv comment7 pages, including 2 figures. To appear in proceedings of IAU Symposium No. 243: Star-Disk Interaction in Young Stars
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