Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....39..113q&link_type=abstract
Astronomy and Astrophysics, vol. 39, no. 1, Feb. 1975, p. 113-125.
Astronomy and Astrophysics
Astrophysics
31
Astronomical Models, Atmospheric Models, Late Stars, Stellar Atmospheres, Stellar Spectra, Cool Stars, Line Spectra, Molecular Spectra, Nuclear Fusion, Stellar Temperature
Scientific paper
A series of models for the atmospheres of cool stars are given. The temperature range is 2600 to 3800 K, and the gravity is taken as 0.1, 1, or 10. Line blanketing by CO, CN and C2 is handled by the OPDF method. The multiple component OPDF is shown to be rather better in so far as a correct emergent flux is concerned. The chemical compositions are those to be expected from the 3alpha-process. Each different chemical composition leads to different sets of spectral lines, and to different strengths of the same lines: the chemical composition therefore affects the distribution of opacity in a stellar atmosphere and thereby affects the distribution of cooling and back-warming regions for a given gravity and effective temperature. The partial pressures of diatomic and polyatomic molecules allow us to determine which molecules typify the different kinds of atmospheres which can be built up out of the elemental abundances predicted by nucleosynthesis.
Querci Francois
Querci Monique
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