Statistics – Computation
Scientific paper
Aug 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...202..159r&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 202, no. 1-2, Aug. 1988, p. 159-162.
Statistics
Computation
17
Computational Astrophysics, Line Spectra, Stellar Atmospheres, Atomic Spectra, Doppler Effect, Hot Stars, Nonequilibrium Thermodynamics, Stark Effect
Scientific paper
Pure-hydrogen non-LTE model atmospheres appropriate for very hot stars (33,000K ≤ Teff ≤ 100,000K and 4 ≤ log g ≤ 7) are examined for the effects of approximations commonly used in model and line formation calculations. First, the authors determine the number of non-LTE levels and line transitions which have to be accounted for, in order to yield the numerical accuracy necessary for analyses of modern high resolution high S/N spectra. Then they investigate the spectral discretization of the radiation field within the lines. Finally, the assumption of pure thermal Doppler broadening when calculating rate equations is checked for its adequacy. It is shown that Stark broadened absorption coefficients yield essentially the same results as the Doppler profiles.
Rauch Thomas
Werner Kirstin
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