Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...243..954w&link_type=abstract
Astrophysical Journal, Part 1, vol. 243, Feb. 1, 1981, p. 954-969.
Physics
19
Early Stars, Hot Stars, Radiation Pressure, Radiative Transfer, Stellar Models, Stellar Winds, Acceleration (Physics), Line Spectra, Optical Thickness, Spectral Energy Distribution
Scientific paper
The line transfer equation in the fluid frame is solved to evaluate radiation pressure force, and a hydrodynamic structure consistent with this force is constructed for stellar wind models driven by radiation pressure in spectral lines. The models use either a number of driving lines of equal length or several lines with different opacities, which are weighed to simulate a distribution of line strengths. An acceleration near the base of the wind that is more gradual than that of the Castor, Abbott, Klein (1975) model was found even well above the sonic point, though mass-loss rates and wind structure at large radii are in substantial agreement with earlier results.
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