Astronomy and Astrophysics, volume 442, 635-642 (2005/11-1)
Metallicity of M dwarfs. I. A photometric calibration and the impact on the mass-luminosity relation at the bottom of the main sequence.
BONFILS X., DELFOSSE X., UDRY S., SANTOS N.C., FORVEILLE T. and SEGRANSAN D.
Abstract (from CDS):
We obtained high resolution ELODIE and CORALIE spectra for both components of 20 wide visual binaries composed of an F-, G- or K-dwarf primary and an M-dwarf secondary. We analyse the well-understood spectra of the primaries to determine metallicities ([Fe/H]) for these 20 systems, and hence for their M dwarf components. We pool these metallicities with determinations from the literature to obtain a precise (±0.2dex) photometric calibration of M dwarf metallicities. This calibration represents a breakthrough in a field where discussions have had to remain largely qualitative, and it helps us demonstrate that metallicity explains most of the large dispersion in the empirical V-band mass-luminosity relation. We examine the metallicity of the two known M-dwarf planet-host stars, Gl 876
(+0.02dex) and Gl 436
(-0.03dex), in the context of preferential planet formation around metal-rich stars. We finally determine the metallicity of the 47 brightest single M dwarfs in a volume-limited sample, and compare the metallicity distributions of solar-type and M-dwarf stars in the solar neighbourhood.
techniques: spectroscopic - stars: abundances - stars: late-type - binaries: visual - planetary systems - stars: individual: Gl 876, Gl 436
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