An investigation into the nature of the symbiotic stars

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Binary Stars, S Stars, Stellar Models, Symbiosis, Main Sequence Stars, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Motions, Stellar Spectra, Ultraviolet Spectra

Scientific paper

A sample of twelve symbiotic variables were examined using both low and high resolution ground-based and satellite observations. The majority of the stars were quiescent stellar, or S-type, systems; observations were also obtained for CH Cygni, AX Persei and AG Draconis during or following their respective 1977, 1978 and 1980 eruptions. High resolution photoelectric Zeeman spectra of AG Pegasi and EG Andromedae failed to find confirming evidence for coherent surface magnetic fields; similar data for CH Cyg following the 1977 eruption also indicated such fields are not present at outburst, thus weakening the single star magnetic model. Contemporaneous optical and ultraviolet spectra for AG Peg yielded revised estimates for the orbital parameters. Composite continuum energy distributions were derived for ten stars from 1200 A to 3.4 microns. The role of accretion in the symbiotics remains uncertain. Accretion models posit a main sequence accretor in order to explain the lack of a significant soft X-ray flux. The models for AG Peg and AG Dra, however, indicate the primaries are subluminous evolved stars, similar to the central objects of planetary nebulae. These results suggest accretion in the symbiotics may be sporadic, occurring in "bursts', and that at quiescence the accretion disks may dissipate.

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