Model atmospheres for K and M giants

To aid in the interpretations of observations of K and M giant stars, model atmospheres have been calculated, covering the range in effective temperature between 3000 and 4000 K and in surface gravity-log g between 0.0 and 2.0. These models are computed under the usual assumptions of hydrostatic equ...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal. Supplement series 1989-11, Vol.71 (3), p.623-646
Main Authors: Brown, Jeffery A., Johnson, Hollis R., Cutright, Lori C., Alexander, David R., Sharp, Christopher M.
Format: Article
Language:English
Subjects:
640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
ABUNDANCE
Astronomy
ASTROPHYSICS
ATMOSPHERES
CHEMICAL COMPOSITION
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
Earth, ocean, space
ELEMENT ABUNDANCE
EQUILIBRIUM
Exact sciences and technology
GIANT STARS
LTE
MATHEMATICAL MODELS
SPECTRA
STAR EVOLUTION
STAR MODELS
STARS
STELLAR ATMOSPHERES
Stellar atmospheres (photospheres, chromospheres, coronae, magnetospheres). Radiative transfer. Opacity and line formation
Stellar characteristics and properties
Citations: Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:To aid in the interpretations of observations of K and M giant stars, model atmospheres have been calculated, covering the range in effective temperature between 3000 and 4000 K and in surface gravity-log g between 0.0 and 2.0. These models are computed under the usual assumptions of hydrostatic equilibrium, constancy of total (radiative plus convective) flux, and LTE in plane-parallel, horizontally homogeneous geometry. A significant development in these models is the incorporation of an opacity-sampled treatment of absorption by water vapor, which becomes dominant at lower temperatures. The thermal structure and scaling properties of the models are discussed, as are the effects of certain composition changes expected in the course of stellar evolution.
ISSN:0067-0049
1538-4365
DOI:10.1086/191389