High Energy Processes in Young Stars - Recent Results from the Chandra HETGS

Details High Energy Processes in Young Stars - Recent Results from the Chandra HETGS High Energy Processes in Young Stars - Recent Results from the Chandra HETGS

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...20511704s&link_type=abstract

American Astronomical Society Meeting 205, #117.04; Bulletin of the American Astronomical Society, Vol. 36, p.1544

Astronomy and Astrophysics

Astronomy

Scientific paper

The study of high energy signatures from young stars involves a large variety of time scales and dynamical ranges that makes the interpretation of X-ray observations quite difficult. Specifically the study of embedded cluster cores have been almost impossible to study prior to Chandra due to the lack of X-ray resolving power. Within the last five years studies of highly resolved spectra from young stars in cluster cores revealed a broad palette of results and intriguing phenomena for a wide range of stellar mass. One of the intriguing results from the Chandra observations of the Orion Trapezium is that most young early type stars possess hot corona-like spectral signatures, some do not. Similarly young cluster cores, such as the Trifid Nebula or RCW38 seem to confim some of the results found in Orion. Likely more evolved stars, for example in cores of clusters older than 3 Myr as in Tr 37 in IC 1396 or NGC 2362, behave more like the prototype O-starζ Pup. Low-mass T Tauri stars show similarly puzzling enigmas. We present recent data and insights from high resolution X-ray spectroscopy of young stars at evolutionary stages and discuss the emission in the context of various emission mechanisms such involving winds, magnetic confinement, coronae and accretion flows.

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