Shell spectrum of CH CYG at the brightening of the star at the end of 1981

Details Shell spectrum of CH CYG at the brightening of the star at the end of 1981 Shell spectrum of CH CYG at the brightening of the star at the end of 1981

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984afz....20..419l&link_type=abstract

(Astrofizika, vol. 20, May-June 1984, p. 419-428) Astrophysics (ISSN 0571-7132), vol. 20, no. 3, Nov. 1984, p. 225-230. Translat

Astronomy and Astrophysics

Astrophysics

6

Binary Stars, Dwarf Stars, Red Giant Stars, Stellar Spectra, Balmer Series, Line Spectra, Supergiant Stars

Scientific paper

CH Cygni has had a well-developed shell spectrum since the brightening in the fall of 1981. Using two spectrograms with the dispersion 4.2 Å/mm, the shell of the star has been studied. It has been shown that the shell lines are formed around the hot component. The shell ionization temperature 10,000K, electron density 1012cm-3 and the dilution coefficient 10-1- 10-3 have been evaluated from the curve of growth. It has been pointed out that the physical conditions in the accretive shell are close to the conditions in the atmospheres of extremely bright B8 - A2 supergiants.

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