Abstract
Accreting T Tauri stars are observed to be less luminous in X-rays than non-accretors, an effect that has been detected in various star forming regions. To explain this we have combined, for the first time, a radiative transfer code with an accretion model that considers magnetic fields extrapolated from surface magnetograms obtained from Zeeman-Doppler imaging. Such fields consist of compact magnetic regions close to the stellar surface, with extended field lines interacting with the disk. We study the propagation of coronal X-rays through the magnetosphere and demonstrate that they are strongly absorbed by the dense gas in accretion columns.
Original language | English |
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Title of host publication | Star-Disk Interaction in Young Stars |
Subtitle of host publication | Proceedings of the International Astronomical Union |
Editors | J. Bouvier, I. Appenzeller |
Publisher | Cambridge University Press |
Pages | 163-170 |
Number of pages | 8 |
Volume | 243 |
DOIs | |
Publication status | Published - May 2007 |