Statistical Procedure for Computing Line-Blanketed Model Stellar Atmospheres.
Abstract
In order to treat the problem of line blanketing in computing model stellar atmospheres we have developed a modified picket-fence approach. We divide the frequency range between the Lyman limit and 44 000 A into 16 separate regions and for each of these regions we compute at 34 optical depths a function N (H). This function descril~es the number distribution of the ratio of line to continuum opacity H. It is computed using a compilation of transition probabilities and excitation potentials for 28 500' spectral lines. The function N(H) is used to choose five values of H for each frequency region. Corresponding to each H is the fraction W of the particular frequency region occupied by opacity ratios equal to or less than H. The values of H and W for each frequency region and the continuum opacities are then used as input to a modified version of the stellar atmosphere program discussed by Strom and Avrett (Astrophys. J. Siippl. 12,1, 1965). We have tested the numerical accuracy of our program by comparing with the results obtained by Avrett for a grey atmosphere and a simple picket- fence absorption coefficient. Finally, we discuss the use of this program for the analysis of Procyon.
- Publication:
-
The Astronomical Journal
- Pub Date:
- 1966
- DOI:
- 10.1086/110142
- Bibcode:
- 1966AJ.....71S.181S