THE INFLUENCE OF H2O LINE BLANKETING ON THE SPECTRA OF COOL DWARF STARS.
L39 - L41.
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.
|Title:||THE INFLUENCE OF H2O LINE BLANKETING ON THE SPECTRA OF COOL DWARF STARS|
|Keywords:||MOLECULAR DATA, STARS, LOW-MASS, BROWN DWARFS, WATER|
|UCL classification:||UCL > School of BEAMS > Faculty of Maths and Physical Sciences
UCL > School of BEAMS > Faculty of Maths and Physical Sciences > Physics and Astronomy
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