Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...167..304e&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 167, Oct. 1986, p. 304-310. Research supported by the Naturvetenskapliga Forsk
Astronomy and Astrophysics
Astrophysics
27
Carbon Stars, Line Spectra, Stellar Atmospheres, Stellar Models, Algorithms, Data Correlation, Opacity
Scientific paper
A comparison of opacity sampling (OS) and opacity distribution function (ODF) methods for the calculation of the model atmospheres of carbon stars is presented. In order to determine the structure of OS model atmospheres to an accuracy of about 30 K or better, at least 5000 frequency points with a near optimum distribution are found to be necessary. The ODF approximation is shown to cause significant errors, particularly where polyatomic opacity dominates in the surface layers, and the diatomic molecules at larger depths. The noncorrelation assumption is not found to lead to significant errors, even for very cool and carbon rich stars. Good agreement is found between multiple component ODF models and ODF models calculated using the ODF-summation procedure of Saxner and Gustafsson (1984) for single component ODFs.
Ekberg U.
Eriksson Kimmo
Gustafsson Bengt
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