Volume 396, Number 3, December IV 2002
|Page(s)||967 - 975|
|Section||Stellar structure and evolution|
|Published online||05 December 2002|
Carbon monoxide bands in M dwarfs
Main Astronomical Observatory of Academy of Sciences of Ukraine, Golosiiv woods, Kyiv-127, 03680 Ukraine e-mail: email@example.com
2 Astrophysics Research Institute, Liverpool John Moores University, Egerton Wharf, Birkenhead CH41 1LD, UK e-mail: firstname.lastname@example.org
Corresponding author: Ya. V. Pavlenko, email@example.com
Accepted: 30 September 2002
We compare the observational and theoretical spectra of the CO bands in a range of M dwarfs. We investigate the dependence of theoretical spectra on effective temperatures as well as carbon abundance. In general we find that the synthetic CO bands fit the observed data extremely well and are excellent diagnostics. In particular the synthetic spectra reasonably match observations and the best fit temperatures are similar to those found by empirical methods. We also examine the 12C/13C isotopic ratio. We find that fundamental 13CO bands around 2.345 and 2.375 μm are good discriminators for the 12C/13C ratio in M dwarfs. The 2.375 μm band is more useful because it doesn't suffer such serious contamination by water vapour transitions. Our current dataset does not quite have the wavelength coverage to perform a reliable determination of the 12C/13C ratio in M dwarfs. For this we recommend observing the region 2.31–2.40 μm at a resolution of better than 1000. Alternatively the observational problems of contamination by water vapour at 2.345 μm maybe solved by observing at resolutions of around 50 000. We also investigated the possibility of using the = 1 CO bands around 4.5 μm. We find that the contamination due to water vapour is even more of a problem at these wavelengths.
Key words: stars: fundamental parameter
© ESO, 2002
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