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

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

Research output: Contribution to journalArticlepeer-review

43 Citations (Scopus)

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 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
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society
Volume379
DOIs
Publication statusPublished - 21 Jul 2007

Keywords

  • stars : activity
  • stars : coronae
  • stars : magnetic fields
  • stars : pre-main sequence
  • X-rays : stars
  • ORION NEBULA CLUSTER
  • MAIN-SEQUENCE STARS
  • MAGNETIC-FIELDS
  • MAGNETOSPHERIC ACCRETION
  • ULTRADEEP PROJECT
  • YOUNG STARS
  • EMISSION
  • ROTATION
  • INSIGHTS
  • OBJECTS

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