Structure of the expanding atmosphere of P Cygni

Details Structure of the expanding atmosphere of P Cygni Structure of the expanding atmosphere of P Cygni

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.106..341a&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 106, no. 2, Nov. 1984, p. 341-353.

Astronomy and Astrophysics

Astrophysics

4

Stellar Atmospheres, Stellar Structure, Supergiant Stars, Spectrum Analysis, Stellar Envelopes, Stellar Mass Ejection

Scientific paper

With the aid of spectra taken in the years 1959 - 1968, a physical analysis of the atmosphere of P Cygni has been carried out and the motions of the atmosphere have been studied. The variations of radial velocities, the velocity progressions of Balmer and He I lines, the high rate of mass loss (2×10-5M_sun;yr-1), the features of the observed line profiles, especially that of H - K lines of Ca II and D1 - D2 lines of Na I confirm the conclusion of Van Blerkom (1978), concerning the assumption of an accelerating atmosphere for P Cygni. An atmospheric model based on the assumption of three envelopes, two of which accelerate gradually with two different velocity laws (up to 11.2 rc), and the third of which accelerates rapidly with a standard velocity law (beyond 11.2 rc) has been developed.

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