Formation of Line Profile : SEI method

Details Formation of Line Profile : SEI method Formation of Line Profile : SEI method

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996jkas...29...93c&link_type=abstract

Journal of the Korean Astronomical Society, vol. 29, no. 2, p. 93-105

Mathematics

Probability

1

P-Cygni Profile, Radiative Transfer, Sobolev Approximation, Escape Probability

Scientific paper

We have solved the radiative transfer problem using a Sobolev approximation with an escape probability method in case of the supersonic expansion of a stellar envelope to an ambient medium. The radiation from the expanding envelope turns out to produce a P-Cygni type profile. In order to investigate the morphology of the theoretical P-Cygni type profile, we have treated Vinf, Vsto, beta(parameters for the velocity field), Mdot, and epsillon(parameter for collisional effect) as model parameters. We have investigated that the velocity field and the mass loss rate affect the shapes of the P-Cygni type profiles most effectively. The secondarily important factors are Vinf, Vsto. The collisional effect tends to make the total flux increased but not so much in magnitude. We have infered some physical parameters of 68 Cyg, HD24912, and Xi persei such as Vinf, Mdot from the model calculation, which shows a good agreement with the observational results.

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