Orbital Radial Velocity Curves of Symbiotic Stars
For the past 6 years we have been measuring the radial velocity of the M-giant component of Symbiotics Stars with high dispersion echelle spectrographs. Because these velocities are based on the absorption line spectrum of the M-star, very reliable orbital radial velocity curves can be constructed. The orbital solutions derived from these velocity curves allow the approximate size of the binary to be determined, and also provide insight into the origin of the photometric variations seen in these stars. For most of the stars, the photometric variations are due to eclipse or reflection effects (two notable exceptions are Z And and RW Hya). Stars which may be near to filling their Roche lobes are TX CVn, Z And, EG And, UV Aur, and CI Cyg. Stars which do not appear to fill their Roche lobes are AG Dra, RW Hya, and AG Peg.
Unable to display preview. Download preview PDF.
- Aller, L.H., Publ. DAO Victoria, B.C., 9, 321.Google Scholar
- Huang, C.C., 1983, in IAU Colloquium No. 70, The Nature of Symbiotic Stars ,ed. M. Fried jung and R. Viotti, (Dordrecht:Reidel), p. 151.Google Scholar
- Mirzoyan, L.V., and Bartaya, R.A., 1960, Izv. Abastumani Astrofiz. Obs. ,No. 25, 121.Google Scholar
- Meinunger, L., 1981, Inf. Bull. Var. Stars ,No. 2016.Google Scholar
- Meinunger, L., 1979 Inf. Bull. Var. Stars ,No. 1611.Google Scholar
- Payne-Gaposchkin, C., 1957, The Galactic Novae (Amsterdam: North Holland).Google Scholar