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The influence of H2O line blanketing on the spectra of cool dwarf starsWe 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.
Document ID
19950034056
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Allard, F. (Univ. of British Columbia Vancouver, British Colum., Canada)
Hauschildt, P. H. (Arizona State Univ. Tempe, Arizona, United States)
Miller, S. (Univ. College London London, United Kingdom)
Tennyson, J. (Univ. College London London, United Kingdom)
Date Acquired
August 16, 2013
Publication Date
May 1, 1994
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters
Volume: 426
Issue: 1
ISSN: 0004-637X
Subject Category
ASTRONOMY
Distribution Limits
Public
Copyright
Other