The influence of H2O line blanketing on the spectra of cool dwarf stars

Details The influence of H2O line blanketing on the spectra of cool dwarf stars The influence of H2O line blanketing on the spectra of cool dwarf stars

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426l..39a&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 426, no. 1, p. L39-L41

Astronomy and Astrophysics

Astrophysics

65

Absorption Spectra, Atmospheric Composition, Atmospheric Models, Brown Dwarf Stars, Cool Stars, Infrared Spectra, Molecular Spectra, Opacity, Stellar Atmospheres, Stellar Composition, Stellar Models, Stellar Spectra, Water, Astronomical Spectroscopy, Electron Energy, Infrared Spectroscopy, Spectrum Analysis

Scientific paper

We present our initial results of model atmosphere calculations for cool M dwarfs using an opacity sampling method and a new list of H2O lines. We obtain significantly improved fits to the infrared spectrum of the M dwarf VB10 when compared to earlier models. H2O is by far the dominant opacity source in cool stars. To illustrate this, we show the Rosseland mean of the total extinction under various assumptions. Our calculations demonstrate the importance of a good treatment of the water opacities in cool stars and the improvements possible by using up-to-date data for the water line absorption.

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