Metallicity determination of M dwarfs⋆

Author： Lindgren Sara   Heiter Ulrike  

Publisher： Edp Sciences

E-ISSN： 1432-0746|604|issue|A97-A97

ISSN： 0004-6361

Source： Astronomy & Astrophysics, Vol.604, Iss.issue, 2017-08, pp. : A97-A97

Disclaimer: Any content in publications that violate the sovereignty, the constitution or regulations of the PRC is not accepted or approved by CNPIEC.

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Abstract

Context. Reliable metallicity values for late K and M dwarfs are important for studies of the chemical evolution of the Galaxy and advancement of planet formation theory in low-mass environments. Historically it has been challenging to determine the stellar parameters of low-mass stars because of their low surface temperature, which causes several molecules to form in the photospheric layers. In our work we use the fact that infrared high-resolution spectrographs have opened up a new window for investigating M dwarfs. This enables us to use similar methods as for warmer solar-like stars.

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