Accretion and Outflow-Related X-Rays in T Tauri Stars

Abstract

We report on accretion- and outflow-related X-rays from T Tauri stars, based on results from the "XMM-Newton Extended Survey of the Taurus Molecular Cloud." X-rays potentially form in shocks of accretion streams near the stellar surface, although we hypothesize that direct interactions between the streams and magnetic coronae may occur as well. We report on the discovery of a "soft excess" in accreting T Tauri stars supporting these scenarios. We further discuss a new type of X-ray source in jet-driving T Tauri stars. It shows a strongly absorbed coronal component and a very soft, weakly absorbed component probably related to shocks in microjets. The excessive coronal absorption points to dust-depletion in the accretion streams.

8 pages, 9 figures, in press, Proc. IAUS 243, Star-Disk Interactions in Young Stars

References in corpus (11)

• The Origin of T Tauri X-ray Emission: New Insights from the Chandra Orion Ultradeep Project
• Evidence for Accretion: High-Resolution X-ray Spectroscopy of the Classical T Tauri Star TW Hydrae
• Chandra Orion Ultradeep Project: Observations and Source Lists
• A Multiwavelength Study of Star Formation in the L1495E Cloud in Taurus
• Evidence for an X-Ray Jet in DG Tau A?
• The X-ray Luminosities of HH Objects
• X-ray Emission from Orion Nebula Cluster Stars with Circumstellar Disks and Jets
• X-rays from HH 80, HH 81, and the Central Region
• A High-Resolution Very Large Array Observation of a Protostar in OMC-3: Shock-induced X-ray Emission by a Protostellar Jet
• The Unusual X-ray Spectrum of FU Orionis
• X-rays from Cepheus A East and West