A simplified method for calculation of radiative energy loss due to spectral lines.
Abstract
In problems of atmospheric structure, numerical complexity often precludes exact treatment of the radiative transfer problem, making approximate methods necessary. Such a method, outlined by the author, makes it possible to estimate radiative losses in spectral lines in atmospheres of nonnegligible optical depth. The technique uses approximate solutions of the transfer equation to obtain source functions and photon escape probabilities as a function of position in the atmosphere. An example of the application of this method to hydrogen excitation, ionization, and radiative losses in a solar flare model is presented. The results are then compared with an exact calculation. The method reduces computing time by over four orders of magnitude.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- December 1974
- DOI:
- 10.1086/153265
- Bibcode:
- 1974ApJ...194..483C
- Keywords:
-
- Energy Dissipation;
- Line Spectra;
- Numerical Analysis;
- Radiative Transfer;
- Solar Flares;
- Solar Spectra;
- Atmospheric Models;
- Equilibrium Equations;
- Mathematical Models;
- Probability Theory;
- Solar Atmosphere;
- Solar Physics