An analysis of the published light curves during the 1971 eclipse of 32 Cygni is carried out. In the photosphere of the K-type supergiant component, the opacity slightly decreases with decreasing wavelength between 4000-5500A and increases with decreasing wavelength between 1910-4000A. This wavelength dependence of the opacity is similar to that of the sun. In the chromosphere, the opacity varies with wavelength in the same way as in the photosphere between 2980-5500A while it decreases again at 2460 A and 1910 A. Molecules seem to be the main opacity source in the photosphere at the far-ultraviolet region. In the course of analysis, the colors and radii of the components are determined and the consistency of the values with the luminosities and spectral types are ascertained by other observational data. The spectral type of the B-type component is B S which is later than the B 4 usually accepted. Key words: Atmospheric structure; Eclipsing binaries; Light-curve analysis; Opacity source; Stellar quantities.
Publications of the Astronomical Society of Japan
- Pub Date:
- Atmospheres:Eclipsing Binaries;
- Eclipsing Binaries:Light Curves;
- Opacities:Stellar Atmospheres