The effective temperature and metallicity of CM Draconis

Details The effective temperature and metallicity of CM Draconis The effective temperature and metallicity of CM Draconis

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.291..780v&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 291, p. 780

Astronomy and Astrophysics

Astronomy

25

Binary Stars, Stellar Temperature, Metallicity, Stellar Spectra, Stellar Models, Late Stars, Infrared Stars

Scientific paper

We compare observations of the binary system CM Draconis with synthetic spectra computed using the stellar atmosphere code PHOENIX. Spectroscopic observations from 0.40 to 2.41 microns, combined with photometry and the accurately known surface gravity, enable us to estimate the temperature and metallicity using detailed spectral synthesis. We find discrepancies between the analysis of the IR and optical spectra: while the optical spectral energy distribution (SED) yields a metal-rich solution with Teff of 3000 K, the IR SED yields around 3200 K with (M/H) in the range of -0.8 and -0.6, compatible with the high space motion of the system. The low-metallicity characteristics of the IR SED could be real, and are partly supported by a detailed analysis of the atomic lines in the optical region. Although the known incompleteness of the TiO and H2O line lists in the models used, as well as problems with the observational data, will cause systematic errors, we suggest that CM Draconis could be a chemically peculiar system in that it cannot be modeled with solar abundances.

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