Metallicity and photospheric abundances in field K and M dwarfs

Details Metallicity and photospheric abundances in field K and M dwarfs Metallicity and photospheric abundances in field K and M dwarfs

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.299..753z&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 299, Issue 3, pp. 753-758.

Astronomy and Astrophysics

Astronomy

22

Stars: Abundances, Stars: Activity, Stars: Chromospheres, Stars: Fundamental Parameters, Stars: Late-Type

Scientific paper

Elemental abundances in late-type stars are of interest in several ways: they determine the location of the stars in the HR diagram and therefore their ages, as well as the atmospheric structure in their middle and upper photospheres. Especially in the case of chromospherically active late-type stars the question arises to what degree the upper photosphere is influenced by the nearby chromosphere. Analysing S/N~200 and Deltalambda/lambda~20000 data, we found a mean metallicity index [M/H]=-0.2 for programme K and M field stars based on an analysis of spectra in the region 5500-9000 Angstroms. We also found that the CaI 6162-Angstroms transition is a potential surface gravity indicator for K-type stars. For the chromospheric activity interval 4.4

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