Fraunhofer lines and the structure of stellar atmospheres
Abstract
A review is given on the development of our ideas concerning stellar atmospheres and their spectra. After some brief remarks concerning the early comparisons, between stellar and laboratory spectra it is emphasized that quantitative analysis of stellar spectra must involve essentially three points: (1) spectrophotometric measurements; (2) the theory of radiative and possibly convective transfer; and (3) the atomic theory of absorption coefficients. After following them for the period 1905-1939, the more recent developments are characterized by treating radiative transfer in spectral lines mostly according to the scheme of "true absorption" and by giving closer attention to the temperature-stratification, using essentially non-grey models. Finally, the importance of more and better theoretical, and particularly laboratory work on transition probabilities, line broadening, etc., is stressed. The problem of damping constants in solar type stars is given special attention.
- Publication:
-
Vistas in Astronomy
- Pub Date:
- 1955
- DOI:
- 10.1016/0083-6656(55)90033-7
- Bibcode:
- 1955VA......1..249U