The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution

Several methods have been proposed for correcting the temperature distribution in the calculation of model stellar atmospheres. The usually efficient procedure of Avrett and Krook (1963) has been widely used, although it may be superseded in some cases by the Auer and Mihalas (1968) method. Recently...

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Detalles Bibliográficos
Autores principales: Rohrmann, René, Milone, L.A.
Formato: Articulo Comunicacion
Lenguaje:Español
Publicado: 1992
Materias:
Astronomía
Galaxia
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/143629
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-143629
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Español
topic Astronomía
Galaxia
spellingShingle Astronomía
Galaxia
Rohrmann, René
Milone, L.A.
The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
topic_facet Astronomía
Galaxia
description Several methods have been proposed for correcting the temperature distribution in the calculation of model stellar atmospheres. The usually efficient procedure of Avrett and Krook (1963) has been widely used, although it may be superseded in some cases by the Auer and Mihalas (1968) method. Recently, still another procedure was proposed (Simonneau and Crivellari, 1988) which deserves further consideration. For our analysis we selected a method due to Napier and Dodd (1974) because it admits a rather simple numerical implementation. Also, as we were primarily interested in such things as how fast the method leads to final values, whether these values are the correct ones, and the dependence of the results on the initial temperature distribution, we simply considered a RE and LTE atmosphere, only affected by H and H⁻ continuous absorption. A special procedure was devised for calculating the flux as accurately as necessary. Three models were calculated, from Tₑ=10000K and g=10000cm/seg², to solar conditions, and standard optical depth ranging from 1E-4 to 100 (standard optical depth was selected at λ2000, or λ5000, according to model). The temperature distribution was represented using a Chebyshev polinomial expansion, and using sixth order approximation, a flux constancy better than 3% was obtained; the inclusion of more than 6 polinomials does not assure a better result. The convergence is rather fast: only 4 or 5 iterations are necessary.
format Articulo
Comunicacion
author Rohrmann, René
Milone, L.A.
author_facet Rohrmann, René
Milone, L.A.
author_sort Rohrmann, René
title The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
title_short The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
title_full The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
title_fullStr The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
title_full_unstemmed The calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
title_sort calculation of model stellar atmospheres: analysis of a method for correcting the temperature distribution
publishDate 1992
url http://sedici.unlp.edu.ar/handle/10915/143629
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