X-Ray Spectra of Cool and Hot Stars Obtained by Chandra and XMM-Newton

Details X-Ray Spectra of Cool and Hot Stars Obtained by Chandra and XMM-Newton X-Ray Spectra of Cool and Hot Stars Obtained by Chandra and XMM-Newton

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005phst..119...13r&link_type=abstract

Physica Scripta, Volume T119, pp. 13-19 (2005).

Physics

Scientific paper

This paper gives an overview of the possibilities and diagnostic tools in analysing x-ray spectra of stellar coronae of cool stars and of colliding winds in hot star (binary) systems. Cool and hot stars show very line-rich x-ray spectra. The spectra are dominated by iron lines (from Fe IX - Fe XXV) and by transitions of H- and He-like C, N, O, Ne, Mg, Si, S, and Ar. In cool stars the n = 2 to n = 1 He-like transitions serve as strong diagnostic tools for the temperature as well as for the density, while for hot stars the strong radiation field mimics a high density. For hot stars these transitions offer the possibility to determine the position of the plasma in relation to the stellar surface. Using the SPEX-code in combination with MEKAL, Multi-Temperature Fitting to the x-ray spectra as a whole results in values for the dominant temperatures, emission measures, and abundances.

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