Stellar Coronal Spectroscopy with the Chandra HETGS

David P. Huenemoerder, Massachusetts Institute of Technology
Bram Boroson, Massachusetts Institute of Technology
Norbert S. Schulz, Massachusetts Institute of Technology
Claude R. Canizares, Massachusetts Institute of Technology
Derek L. Buzasi, U.S. Air Force Academy, Colorado Springs
Heather L. Preston, U.S. Air Force Academy, Colorado Springs
Joel H. Kastner, Rochester Institute of Technology

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.


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.