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.
|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|
|Number of pages||8|
|Publication status||Published - May 2007|