Coronal X-Ray Spectroscopy of Solar Analogs

Details Coronal X-Ray Spectroscopy of Solar Analogs Coronal X-Ray Spectroscopy of Solar Analogs

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..219..930t&link_type=abstract

Stars as suns : activity, evolution and planets, Proceedings of the 219th symposium of the International Astronomical Union held

Physics

Scientific paper

We present an X-ray study of a series of solar-mass main-sequence stars with different ages based on data from XMM-Newton and Chandra. This investigation aims at a closer understanding of the physical mechanisms of heating and mass transport in magnetically active stars. All targets are proxies of the Sun that essentially differ only in their rotation periods and hence in the efficiency of the magnetic dynamo. We present a spectral analysis that constrains the average elemental composition and the thermal structure of the coronae at different stages of their evolution. Further we use the He-like line triplets to derive characteristic coronal densities and investigate the time variability in the X-ray light curves. We discuss implications for models related to heating physics and coronal structure.

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