Observational studies of the symbiotic stars. II Emission-line relative intensity variations in CI Cygni, BF Cygni, AX Persei, and V1016 Cygni

Details Observational studies of the symbiotic stars. II Emission-line relative intensity variations in CI Cygni, BF Cygni, AX Persei, and V1016 Cygni Observational studies of the symbiotic stars. II Emission-line relative intensity variations in CI Cygni, BF Cygni, AX Persei, and V1016 Cygni

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...268..250o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 268, May 1, 1983, p. 250-263.

Astronomy and Astrophysics

Astrophysics

22

Binary Stars, Stellar Models, Stellar Spectra, Stellar Spectrophotometry, Variable Stars, Companion Stars, High Resolution, Line Spectra, Spectral Resolution, Stellar Luminosity

Scientific paper

Low-resolution spectra (λλ3800-5900) are presented of the symbiotic stars CI Cygni, BF Cygni, AX Persei, and V1016 Cygni, which were obtained with the Washburn Observatory Boller and Chivens cassegrain spectrograph and intensified Reticon. The spectra were obtained as part of a monitoring program covering 36 months since 1978 November. These data are used in conjunction with ultraviolet spectra from the archives of International Ultraviolet Explorer data. The nebular electron temperature and density are derived from the [O III] λ5007 and λ4363 emission lines and the UV intercombination lines of λ1661 and λ1667. Relative emission-line intensity variations were observed in all four stars. The relative emission line changes correlated with photometric minima for CI Cyg, AX Per, and possibly BF Cyg. These changes are interpreted as due to a red giant eclipsing a nebula surrounding the exciting source. Based on the [O III] line ratio change, the nebular density of V1016 Cyg has continued to decline since 1978.
A decline in the intensity ratios of [Ne III] λ3869 to [O III] and He I λ5876 to [O III] λ5007 were also observed during the 1980 minimum of CI Cyg. The observed I(3869)/I(5007) decline was too large to be explained by temperature, density, or abundance changes. The Ne++ and He+ emission regions are therefore closer to the hot source than the more extended [O III] emission region.

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