Stellar Coronal Spectroscopy with the Chandra HETGS
This is the pre-print of a paper published by the Astronomical Society of the Pacific.
Published in: Stars as suns : activity, evolution and planets, Proceedings of the 219th symposium of the International Astronomical Union held during the IAU General Assembly XXV, Sydney, Australia, 21-25 July 2003
© 2003 Astronomical Society of the Pacific
Support for this work was provided by NASA contract NAS8-01129, SAO SV1-61010 (CXC/MIT), and NASA-Chandra Award Number G02-3005A issued by the CXC, which is operated by SAO for and on behalf of NASA under contract NAS8-39073. We also thank the Air Force Office of Scientific Research for their support.
Also archived in: arXiv: astro-ph/0310319 v1 11 Oct 2003
Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.
Description
Spectroscopy with the Chandra High Energy Transmission Grating Spectrometer (HETGS) provides details on X-ray emission and activity from young and cool stars through resolution of emission lines from a variety of ions. We are beginning to see trends in activity regarding abundances, emission measures, and variability. Here we contrast spectra of TV Crt, a weak-lined T Tauri star (WTT), with TW Hya, a Classical T Tauri star (CTT). TV Crt has a spectrum more like magnetic activity driven coronae, relative to the TW Hya spectrum, which we have interpreted as due to accretion-produced X-rays. We have also observed the long period system, IM Pegasi to search for rotational modulation, and to compare activity in a long period active binary to shorter period systems and to the pre-main sequence stars. We detected no rotational modulation, but did see long-duration flares.
