Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21533501s&link_type=abstract
American Astronomical Society, AAS Meeting #215, #335.01; Bulletin of the American Astronomical Society, Vol. 42, p.434
Astronomy and Astrophysics
Astronomy
1
Scientific paper
We present the analysis of Chandra X-ray observations of a sample of young stars, particularly T Tauri stars, in order to better understand the characteristics of the X-ray emitting plasmas of young stars and the physical mechanisms that produce that emission. Our sample includes Chandra High Energy Transmission Grating Spectroscopy (HETGS) relatively long integration, high spectral resolution data for nine young stars, including classical, weak-lined, and post-T Tauri stars as well as a young main sequence star. For five of these nine stars we observed significant flaring during the Chandra observing epochs. We extracted spectra for each observation, and for the observations with significant flaring, we extracted separate spectra for the flaring and quiescent epochs. From these spectra, we measured the line fluxes of the strongest emission lines, most notably the Hydrogen-like Lyman line and the He-like triplet (forbidden, intercombination, and resonance) lines for Si, Mg, and Ne as well as strong Fe lines. From these line flux measurements, we were able to infer densities and temperatures from line flux ratios sensitive to these properties. In general, the quiescent state observations have higher densities (as inferred by the density-sensitive R ratio) than the flaring state observations. By measuring elemental abundance ratios, we find that all the observations of the stars in our sample have a high Ne/Fe ratio, but only one, TW Hya in quiescence, shows an enhanced Ne/O ratio. This work was supported by a grant from NASA's Chandra X-ray Observatory.
Shukla Sonali J.
Weintraub David
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