Model Solar Atmospheres.
Abstract
An iteration method is described for obtaining model stellar atmospheres when the temperature as a function of optical depth is known. This process is applied to the solar atmosphere, using an empirical temperature distribution based on observations of limb darkening. The total pressure, the electron pressure, and the absorption coefficient are tabulated as functions of the optical depth for different hydrogento-metal ratios. In addition, two solar models with He/H ratios of and are tabulated and compared with other models.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 1952
- DOI:
- 10.1086/145601
- Bibcode:
- 1952ApJ...116..176A