Mass transfer and line profiles - WZ SGE

Details Mass transfer and line profiles - WZ SGE Mass transfer and line profiles - WZ SGE

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.130..151s&link_type=abstract

(IAU, DFG, and Bayerisches Staatsministerium für Unterricht und Kultus, Colloquium on Cataclysmic Variables, Recent Multi-Freque

Astronomy and Astrophysics

Astrophysics

4

Accretion Disks, Cataclysmic Variables, Line Spectra, Stellar Mass Accretion, Stellar Spectra, Mass Transfer, Starspots

Scientific paper

Using the method of Hadrava (1984), the behavior of the gaseous stream of WZ Sge is calculated, and the line profiles caused by the disk are determined. It is found that the ratio of the geometrical thickness of the stream and of the disk are dependent on the temperature regime of the stream in addition to the accretion regime of the disk. The linear approximation of the stream of Sima (1979) is found to be plausible. The stream in WZ Sge cannot be optically detected. The ring is shown to produce two emission peaks in the line profile, while the rotating white dwarf produces a broad absorption.

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