Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21822105b&link_type=abstract
American Astronomical Society, AAS Meeting #218, #221.05; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astrophysics
Scientific paper
Young stellar objects exhibit X-ray emission throughout their evolution. The emission above about 1 keV is primarily produced from coronal structures and flares, indicating that magnetic activity is present from early on. For stars that are still actively accreting, X-ray accretion signatures of accretion are only distinguishable at
low energies in high resolution grating spectra from Chandra and XMM-Newton. The accretion shock itself is identified in only a few of these sources through line ratio diagnostics for high electron density at relatively low temperature. However, a soft X-ray excess, compared with main sequence and weak-line T Tauri stars, is found in all the Classical T Tauri grating targets. This emission presents as excess O VII. Exactly what produces the soft excess and how it relates to the
shock and to the photospheric accretion hot spot is unclear without additional diagnostics. Shocks in jets and winds, as well as magnetic heating at the hot spot are possible. High resolution soft X-ray spectroscopy will allow us to determine the velocity structure from
line profiles, the density and volume from line diagnostics for a range of soft X-ray emitting temperatures, and the absorbing column density of pre-shock gas as a function of shock structure. The author's work is supported by the Chandra X-ray Observatory through a NASA contract with the Smithsonian Astrophysical Observatory.
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