Rotationally modulated X-ray emission from T Tauri stars

S. G. Gregory, M. Jardine, A. Collier Cameron, J. -F. Donati

Research output: Contribution to journalArticle

24 Citations (Scopus)

Abstract

We have modelled the rotational modulation of X-ray emission from T Tauri stars assuming that they have isothermal, magnetically confined coronae. By extrapolating surface magnetograms, we find that T Tauri coronae are compact and clumpy, such that rotational modulation arises from X-ray emitting regions being eclipsed as the star rotates. Emitting regions are close to the stellar surface and inhomogeneously distributed about the star. However, some regions of the stellar surface, which contain wind bearing open field lines, are dark in X-rays. From simulated X-ray light curves, obtained using stellar parameters from the Chandra Orion Ultradeep Project, we calculate X-ray periods and make comparisons with optically determined rotation periods. We find that X-ray periods are typically equal to, or are half of, the optical periods. Further, we find that X-ray periods are dependent upon the stellar inclination, but that the ratio of X-ray to optical period is independent of stellar mass and radius.
Original languageEnglish
Pages (from-to)827-835
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Volume373
Issue number2
DOIs
Publication statusPublished - 30 Oct 2006

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