Spectroscopic Orbit of the Eclipsing Symbiotic Star CH Cyg
Photometric minima in U light were separated by 5700÷5780 days which is very close to the spectroscopic period (P=5750±250d) found by Yamashita and Maehara (1979) .
Variations of Hβ and Hγ profiles during both minima can be succesfully interpreted as an eclipse of a rotating disk or envelope from which these profiles originate (see also Fernie et al., 1986).
The flickering activity was absent during the 1985 minimum while observed before and after the minimum.
Only forbidden lines were unaffected by the minimum. Recently, additional arguments for the eclipsing nature of CH Cygni have been found:
Deep minimum in the IUE integrated flux was coincided with the minimum detected in U light (Mikołajewska et al., 1987a).
Changes of Balmer decrement and Balmer continuum emission measure suggest a presence of relatively small dense region occulted during the minimum and extended low density region coinciding with the radio jets (Mikołajewska et al., 1987b).
Radial velocity of the jet spatially resolved by Solf (1987) in the [OIII] 5007 line suggests the jet is practically perpendicular to the line of sight.
- Fernie J.D., Lyons R., Beattie B., Garrison R.F.:1986, IBVS No. 2935 Google Scholar
- Mikołajewska J., Selvelli P.L., Hack M. : 1987a, submitted to Astron. Astrophys.Google Scholar
- Mikołajewska J., Mikołajewski M., Biernikowicz R., Selvelli P.L., Turło Z.:1987b, in proceedings of IAU Symp. No. 122, Reidel Co., p. 487Google Scholar
- Yamashita Y., Maehara H.:1979, Publ. Astron. Soc. Japan 31 , 307Google Scholar