Discrete absorption components in spectra of mass-losing stars - an analytical model for the trajectories of gas parcels and streams

Details Discrete absorption components in spectra of mass-losing stars - an analytical model for the trajectories of gas parcels and streams Discrete absorption components in spectra of mass-losing stars - an analytical model for the trajectories of gas parcels and streams

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.223..673b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 223, Dec. 15, 1986, p. 673-681. SERC-supported research

Astronomy and Astrophysics

Astronomy

13

Stellar Mass Ejection, Stellar Models, Stellar Spectra, Stellar Winds, Trajectories, Absorption Spectra, Bipolarity, Photosphere, Stellar Magnetic Fields, Ultraviolet Spectra

Scientific paper

Underhill and Fahey have proposed that the discrete, narrow absorption components which are detected in UV spectra of many mass-losing stars may be caused by the release of parcels of gas from local regions above the stellar photosphere. It is inferred that the release mechanism responsible for this ejection is associated with bipolar magnetic regions on the surface of the star. These authors have given detailed calculations for the trajectory of such gas parcels but because of several approximations made, their model is not of general applicability especially to those stars where the ratio of the tangential velocity of the ejected material to the terminal wind velocity becomes significant. In this paper we give an improved analytical treatment for the trajectory of gas parcels and we discuss also the possible situation where continuous streams of gas may be released from one or more rotating regions above the photosphere. Calculated velocity-time curves for the absorption components are presented for several stars as illustration and we suggest the type of observational requirements which might be used to test the models described.

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