A code for line blanketing without local thermodynamic equilibrium.
Abstract
A numerical code has been written which is designed to calculate radiation transport and atmospheric structure under the constraints of statistical equilibrium in atomic transitions and radiative and hydrostatic equilibrium in the medium. It uses a multi-frequency/multi-grey algorithm which admits the inclusion of many spectral lines in full statistical equilibrium. The program can comfortably accept up to about 300 specific lines arising from about 30 lower states and any number of continua. By way of example, the author presents a model of a stellar atmosphere with effective temperature 35000K and surface gravity 104cm s-2.
- Publication:
-
Progress in Stellar Spectral Line Formation Theory
- Pub Date:
- 1985
- Bibcode:
- 1985ASIC..152..225A
- Keywords:
-
- Line Spectra;
- Radiative Transfer;
- Stellar Atmospheres;
- Thermodynamic Equilibrium;
- Atmospheric Models;
- Computational Astrophysics;
- Electron Energy;
- Astrophysics;
- Line Blanketing:Radiative Transfer;
- Line Blanketing:Stellar Atmospheres;
- Numerical Methods:Radiative Transfer;
- Radiative Transfer:Line Blanketing;
- Radiative Transfer:Numerical Methods;
- Stellar Atmospheres:Line Blanketing