The Coronal Properties of the High-Metallicity G IV-V Star 11 LMi (HD 82885)

Details The Coronal Properties of the High-Metallicity G IV-V Star 11 LMi (HD 82885) The Coronal Properties of the High-Metallicity G IV-V Star 11 LMi (HD 82885)

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008xmm..prop...60d&link_type=abstract

XMM-Newton Proposal ID #06022901

Physics

Stars, White Dwarfs, Solar System, 11 Lmi

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. 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 use XMM-Newton to observe 11 LMi (= HD 82885), a known X-ray source, which has 2.0-2.5 times solar photospheric abundances, in order to study the effect of the high underlying metallicity on the temperature structure and abundances of its coronal plasma.

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