Mass loss from UW Canis Majoris

Details Mass loss from UW Canis Majoris Mass loss from UW Canis Majoris

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....83..363d&link_type=abstract

Astronomy and Astrophysics, vol. 83, no. 3, Mar. 1980, p. 363-369. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

10

Line Shape, O Stars, Stellar Envelopes, Stellar Mass Ejection, Ultraviolet Spectra, Curve Fitting, Electron Energy, Far Ultraviolet Radiation, Mass Flow Rate, Satellite Observation, Supergiant Stars

Scientific paper

The present analysis is an application of the theory described by Lucy (1971) for the calculation of P Cygni resonance line profiles formed by isotropic and coherent scattering in spherically symmetric expanding circumstellar envelopes. Copernicus satellite measurements of resonance features in the FUV spectrum of the O 7 supergiant UW Canis Majoris (= HD 57060) are compared with theoretical P Cygni profiles. Grids of line profiles are computed using four free parameters which contain information about the velocity law, ionization equilibrium, temperature, and envelope density. Thus, with the assumption of a spherically symmetric steady flow, and of solar element abundances, the stellar mass loss rate and the electron temperature of the expanding shell can be derived. The mass flow is treated in a fully transonic way, i.e., the Sobolev approximation is applied.

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