Physics
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........10o&link_type=abstract
Thesis (PH.D.)--THE UNIVERSITY OF WISCONSIN - MADISON, 1982.Source: Dissertation Abstracts International, Volume: 43-04, Sectio
Physics
Scientific paper
Low resolution spectra ((lamda)3800 - (lamda)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 November 1978. The nebular electron temperature and density are derived from the {O III} (lamda)5007 and (lamda)4363 emission lines and the UV intercombination lines of (lamda)1661 and (lamda)1667. 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. The thesis also contains a discussion of the use of the emission lines of {Ne III} (lamda)3869, {O III} (lamda)5007, (lamda)4363 and He I (lamda)5876 to derive nebular electron temperature and density. A decline in the intensity ratios of I((lamda)3869)/((lamda)5007) and I((lamda)5876)/I((lamda)5007) were observed during the 1980 minimum of CI Cyg. The observed I((lamda)3869)/I((lamda)5007) decline was too large to be explained by temperature or density changes. The {Ne III} and He II regions in CI Cyg are therefore closer to the hot source than the more extended {O III} emission region. Contained within the appendix is a discussion of a graphical method of solution of the nebular temperature and density, which is based on the emission lines of {Ne III}, {O III} and He I.
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