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

S. G. Gregory (Lead / Corresponding author), K. Wood, M. Jardine

Research output: Chapter in Book/Report/Conference proceedingConference contribution


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 languageEnglish
Title of host publicationStar-Disk Interaction in Young Stars
Subtitle of host publicationProceedings of the International Astronomical Union
EditorsJ. Bouvier, I. Appenzeller
PublisherCambridge University Press
Number of pages8
Publication statusPublished - 1 May 2007

Publication series

ISSN (Print)1743-9213
ISSN (Electronic)1743-9221


  • Radiative transfer
  • stars: coronae
  • stars: magnetic fields
  • stars: pre-main sequence
  • stars: activity
  • stars: formation
  • X-rays: stars


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