Theoretical line profiles from a symbiotic system

Details Theoretical line profiles from a symbiotic system Theoretical line profiles from a symbiotic system

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.131..707s&link_type=abstract

(IAU, Colloquium on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, 93rd, Bamberg, West

Astronomy and Astrophysics

Astrophysics

3

Cool Stars, Giant Stars, Hot Stars, Line Shape, Stellar Models, Symbiotic Stars, Elliptical Orbits, H Beta Line, Stellar Mass Ejection, Stellar Systems, Stellar Winds

Scientific paper

A model for a symbiotic system is presented which is not spherically symmetrical. The system consists of a cool, mass losing giant and a hot star. The stellar wind from the cool star is radiatively ionized by the hot companion, and the resulting nebular lines are emitted mainly close to the cool star. Due to the elliptical orbit, the line fluxes change with time because of the varying separation of the stars. The line profiles vary from symmetrical to asymmetrical, depending on the angle between the line of sight and the axis of symmetry. The calculated line profiles are compared with observed UV lines of the symbiotic star HBV 475.

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