Statistics – Computation
Scientific paper
Apr 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...327..822h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 327, April 15, 1988, p. 822-839.
Statistics
Computation
113
Carbon Stars, Emission Spectra, Line Spectra, Nitrogen, Wolf-Rayet Stars, Abundance, Computational Astrophysics, Continuous Radiation, Electron Density (Concentration), Stellar Atmospheres, Temperature Distribution
Scientific paper
The author presents a detailed analysis of the formation of the C IV, N IV, and N V lines (both optical and UV) in the extended atmosphere of HD 50896. First, he discusses the basic model for the envelope of HD 50896 as previously found by Hillier (1987). As a prelude to the N and C line formation, he discusses the temperature structure of the envelope. Radiative equilibrium is assumed, and the effect of collisional excitation of nitrogen on the envelope temperature is examined. Simple formulae for the emission equivalent widths of UV resonance lines are derived. These formulae are used to illustrate the basic dependence of the line fluxes on model parameters. Constraints on the C/N, O/N, and N/He abundance ratios are also discussed.
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