The effective temperature and metallicity of CM Draconis
Viti, Serena Jones, Hugh R.A. Schweitzer, Andreas. Allard, France Hauschildt, Peter H. Tennyson, Jonathan Miller, Steven Longmore, Andrew J.
Viti, Serena
Jones, Hugh R.A.
Schweitzer, Andreas.
Allard, France
Hauschildt, Peter H.
Tennyson, Jonathan
Miller, Steven
Longmore, Andrew J.
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1997-11-11
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Keywords
Binaries: spectroscopic,Infrared: stars,Stars: atmospheres,Stars: fundamental parameters,Stars: late-type,Stars: Population II
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Citation
Serena Viti, Hugh R. A. Jones, Andreas Schweitzer, France Allard, Peter H. Hauschildt, Jonathan Tennyson, Steven Miller, Andrew J. Longmore, The effective temperature and metallicity of CM Draconis, Monthly Notices of the Royal Astronomical Society, Volume 291, Issue 4, November 1997, Pages 780–796, https://doi.org/10.1093/mnras/291.4.780
Abstract
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 μm, 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 infrared and optical spectra: while the optical spectral energy distribution (SED) yields a metal-rich solution with Teff = 3000 K, the infrared SED yields around 3200 K with - 0.8 ≤ [M/H] ≤ -0.6, compatible with the high space motion of the system. The low-metallicity characteristics of the infrared 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 modelled with solar abundances. © 1997 RAS.
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This is an open access article under the CC BY license.
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Oxford University Press
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Monthly Notices of the Royal Astronomical Society
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00358711