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Why are accreting T Tauri stars less luminous in X-rays than non-accretors?

Published online by Cambridge University Press:  01 May 2007

S. G. Gregory ,
K. Wood  and
M. Jardine
S. G. Gregory
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK email: [email protected]
K. Wood
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK email: [email protected]
M. Jardine
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK email: [email protected]
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Abstract

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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.

Keywords

Radiative transferstars: coronaestars: magnetic fieldsstars: pre–main-sequencestars: activitystars: formationX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 163 - 170
Copyright
Copyright © International Astronomical Union 2007

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