The Coronal Properties of the High-Metallicity G V Stars 11 LMi and HD 83498

Details The Coronal Properties of the High-Metallicity G V Stars 11 LMi and HD 83498 The Coronal Properties of the High-Metallicity G V Stars 11 LMi and HD 83498

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007xmm..prop...77d&link_type=abstract

XMM-Newton Proposal ID #05523101

Physics

Stars, White Dwarfs, Solar System, 11 Lmi, Xmm-Newton Proposal Id #05523101

Scientific paper

The coronal abundances of late-type stars have been found to show at least 3 different patterns (the First Ionization Potential (FIP) effect, the Inverse-FIP effect, and an intermediate pattern), which appear to be mostly controlled by the level of stellar activity (low, high, and intermediate, respectively). The influence of stellar metallicity on stellar coronal properties is still unclear, since most of the stars with well-studied coronal spectra have photospheric abundances similar to (or assumed to be) the solar photospheric values. We propose to observe 2 stars, both known X-ray sources, which have up to 2 and 5 times solar photospheric abundances, in order to study the effect of the underlying metallicity on the temperature structure and abundances of their coronal plasmas.

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