Why are accreting T Tauri stars less luminous in X-rays than non-accretors?
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.
- Publication:
-
Star-Disk Interaction in Young Stars
- Pub Date:
- May 2007
- DOI:
- 10.1017/S1743921307009520
- arXiv:
- arXiv:0707.0382
- Bibcode:
- 2007IAUS..243..163G
- Keywords:
-
- Radiative transfer;
- stars: coronae;
- stars: magnetic fields;
- stars: pre–main-sequence;
- stars: activity;
- stars: formation;
- X-rays: stars;
- stars: pre-main-sequence;
- Astrophysics
- E-Print:
- 8 pages, 2 figures, to appear in the proceedings of IAU S243: Star-disk Interaction in Young Stars, Grenoble 2007, eds. J. Bouvier and I. Appenzeller