A&A 468, 425-442 (2007)
X-ray emission from T Tauri stars and the role of accretion: inferences from the XMM-Newton extended survey of the Taurus molecular cloudA. Telleschi1, M. Güdel1, K. R. Briggs1, M. Audard2, and F. Palla3
1 Paul Scherrer Institut, Würenlingen and Villigen, 5232 Villigen PSI, Switzerland
2 Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, Mail code 5247, New York, NY 10027, USA
3 INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi, 5, 50125 Firenze, Italy
(Received 13 October 2006 / Accepted 29 November 2006)
Context.T Tau stars display different X-ray properties depending on whether they are accreting (classical T Tau stars; CTTS) or not (weak-line T Tau stars; WTTS). X-ray properties may provide insight into the accretion process between disk and stellar surface.
Aims.We use data from the XMM-Newton Extended Survey of the Taurus molecular cloud (XEST) to study differences in X-ray properties between CTTS and WTTS.
Methods.XEST data are used to perform correlation and regression analysis between X-ray parameters and stellar properties.
Results.We confirm the existence of a X-ray luminosity vs. mass (M) relation, , but this relation is a consequence of X-ray saturation and a mass vs. bolometric luminosity () relation for the TTS with an average age of 2.4 Myr. X-ray saturation indicates = const., although the constant is different for the two subsamples: const. = for CTTS and const. = for WTTS. Given a similar distribution of both samples, the X-ray luminosity function also reflects a real X-ray deficiency in CTTS, by a factor of 2 compared to WTTS. The average electron temperatures are correlated with in WTTS but not in CTTS; CTTS sources are on average hotter than WTTS sources. At best marginal dependencies are found between X-ray properties and mass accretion rates or age.
Conclusions.The most fundamental properties are the two saturation laws, indicating suppressed for CTTS. We speculate that some of the accreting material in CTTS is cooling active regions to temperatures that may not significantly emit in the X-ray band, and if they do, high-resolution spectroscopy may be required to identify lines formed in such plasma, while CCD cameras do not detect these components. The similarity of the vs. dependencies in WTTS and main-sequence stars as well as their similar X-ray saturation laws suggests similar physical processes for the hot plasma, i.e., heating and radiation of a magnetic corona.
Key words: stars: coronae -- stars: formation -- stars: pre-main sequence -- X-rays: stars
© ESO 2007