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

S. G. Gregory, K. Wood, M. Jardine

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43 Citations (Scopus)


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 disc. 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. The reduction in the observed X-ray emission depends on the field geometry, which may explain why accreting T Tauri stars show a larger scatter in their observed X-ray luminosity compared with non-accreting stars.
Original languageEnglish
Pages (from-to)L35-L39
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society: Letters
Issue number1
Publication statusPublished - 1 Jul 2007


  • Stars: activity
  • stars: coronae
  • stars: magnetic fields
  • Stars: pre-main-sequence
  • X-rays: stars

ASJC Scopus subject areas

  • Astronomy and Astrophysics


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