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 L-alpha, L-beta, H-alpha, 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 solar-flare 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