Rotational Modulation of X-ray Emission from T Tauri Stars

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dc.creatorGregory, S. G.
dc.creatorJardine, M.
dc.creatorCameron, A. Collier
dc.creatorDonati, J. -F.
dc.date2007-01-03
dc.date.accessioned2026-07-07T07:38:07Z
dc.date.available2026-07-07T07:38:07Z
dc.descriptionWe have modeled 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.
dc.description3 pages, 4 figures, proceedings of Coronae of Stars and Accretion Disks, Bonn, December 2006, to be published in Memorie della Societa Astronomica Italiana
dc.identifierhttps://arxiv.org/abs/astro-ph/0701060
dc.identifierhttp://arxiv.org/abs/astro-ph/0701060
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/121007
dc.subjectAstrophysics
dc.titleRotational Modulation of X-ray Emission from T Tauri Stars
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