A probabilistic approach to radiative energy loss calculations for optically thick atmospheres  Hydrogen lines and continua
Abstract
An approximate probabilistic radiative transfer equation and the statistical equilibrium equations are simultaneously solved for a model hydrogen atom consisting of three bound levels and ionization continuum. The transfer equation for Lalpha, Lbeta, Halpha, and the Lyman continuum is explicitly solved assuming complete redistribution. The accuracy of this approach is tested by comparing source functions and radiative loss rates to values obtained with a method that solves the exact transfer equation. Two recent model solarflare chromospheres are used for this test. It is shown that for the test atmospheres the probabilistic method gives values of the radiative loss rate that are characteristically good to a factor of 2. The advantage of this probabilistic approach is that it retains a description of the dominant physical processes of radiative transfer in the complete redistribution case, yet it achieves a major reduction in computational requirements.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 1980
 DOI:
 10.1086/158193
 Bibcode:
 1980ApJ...239.1036C
 Keywords:

 Chromosphere;
 H Lines;
 Optical Thickness;
 Radiative Transfer;
 Stellar Atmospheres;
 Approximation;
 Atmospheric Models;
 Energy Dissipation;
 Probability Theory;
 Solar Flares;
 Astrophysics