Sampling Methods

Details Sampling Methods Sampling Methods

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992rmxaa..23..195j&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 23, 195

Statistics

Computation

12

Scientific paper

RESUMEN. El gran aurnento en la capacidad computacional nos lia permitido resolver la ecuacion de transporte radiativo en varios miles de piintos de frecuencia en la sol'ici6n iterativa del modelo atmosf6rico clasico, y construir un muestreo mas detallado y reaifstico de la opacidad que en modelos anteriores. Mientras que la media arm6nica y la media recta permiten un calculo muy rapido de la estriictura del modelo, los errores de estos tratamientos tan simples de Ia. opacidad pueden ser mayores que to dos los errores que resultarfan Si se excluyeran del c6mputo del modelo atmosf6rico de estrellas frfas todos los avances fisicos de los iltimos 25 ailos! Sin embargo, el me'todo mas simple de muestreo basado en la media arm6nica la media de Rosseland -todavfa se utiliza para calcular las condiciones de frontera en los modelos de evoluci6n de las estrellas frias. La transformaci6n estadistica en lineas individuales de los coeficientes de absorci6n media recta que se miden, seguido de `in muestreo cuidadoso, es una mejora considerable sobre el uso corriente del coeficiente de absorci6n media recta en la construcci6n de modelos atmosf6ricos. ABSTRACT. A tremendous increase in computing capacity 1ias allowed us to solve the radiative transfer equation at several thousand frequency points during the iterative solution of the classic model atmosphere problem, and to construct a much more detailed and realistic sampling of the opacity than in earlier models. V,T the harmonic mean and straight mean enable a very fast computation of the model struct `ire, the errors in such simple opacity treatments may be bigger than the errors due to neglect of all improvements in the physics included in computations of model atmospheres of cool stars during the last 25 years! Yet the most simple harmonic mean sampling method the Rosseland mean is often still used to compute boundary conditions for evolutionary models of cool stars. Statistical transformation of measured straight mean absorption coefficients into individual lines, followed by careful sampling, has been a considerable improvement over the direct use of the straight absorption coefficient in the construction of model atmospheres. Key words: OPACITIES - STARS: ATMOSPHERES

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