The long-period symbiotic binary CH Cygni

Details The long-period symbiotic binary CH Cygni The long-period symbiotic binary CH Cygni

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...287..543l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 287, no. 2, p. 543-551

Astronomy and Astrophysics

Astrophysics

11

Accretion Disks, Eclipsing Binary Stars, Emission Spectra, H Alpha Line, Line Spectra, Symbiotic Stars, Eclipses, Stellar Magnetic Fields, Stellar Models, Variable Stars, White Dwarf Stars

Scientific paper

We have analysed H alpha profiles of the peculiar symbiotic star CH Cygni, obtained in 1982-1986 by the 2 m telescope in Rozhen observatory and by the 1.5 m telescope in Tartu observatory. Theoretical emission line profiles from rotating optically thick accretion disk have been computed and compared with the observations. We have found that H alpha profiles of CH Cyg can be considered as arising from a Keplerian disk. Great changes in the line widths are explained as variations of the inner radius of the disk Rin. Such variations are interpreted in the framework of the magnetic rotator model: in 1981-1984 the star was in the accretor state and Rin was about 10 solar radius; it decreased rapidly down to 0.1 solar radius by September 1984, after transition into the propeller state and disruption of the accretion complex around the white dwarf. Afterwards Rin again increased up to 8 solar radius by April 1986. Changes in the H alpha profile show that in 1985 the eclipse of the hot component took place. H alpha line observed in August 1985, probably has its origin in bipolar jets ejected in 1984, it cannot be fitted by the rotational profile with reasonable input parameters.

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