Stellar Coronal Spectroscopy with the Chandra HETGS

Details Stellar Coronal Spectroscopy with the Chandra HETGS Stellar Coronal Spectroscopy with the Chandra HETGS

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hrxs.confe..18h&link_type=abstract

High Resolution X-ray Spectroscopy with XMM-Newton and Chandra, Proceedings of the international workshop held at the Mullard Sp

Computer Science

Scientific paper

Grating spectra of cool stars from Chandra and XMM-Newton reveal a wealth of detail in their emission lines. Ability to resolve lines and detect the continuum allows detailed modeling of the temperature structure, abundances, and sometimes density. The abundances often show anomalies, such as strong neon and weak iron. Line strengths are often anomalous in flux ratios when compared to models or laboratory data. Temperature distributions are highly structured, but differ from star to star. I present qualitative results for a variety of objects: the pre-main sequence star TW Hya, which seems to be accretion driven, to neon-strong, iron-weak and highly variable RS CVn stars, II Peg, TY Pyx, and AR Lac, to the rapidly rotating giant, FK Com. I show detailed emission measures and abundance models for a few objects, as derived from line-based analysis of the coronal X-ray emission.

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