The 1984-1985 optical fade and radio brightening of CH Cygni

Details The 1984-1985 optical fade and radio brightening of CH Cygni The 1984-1985 optical fade and radio brightening of CH Cygni

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986pazh...12..870l&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 12, Nov. 1986, p. 870-877) Soviet Astronomy Letters (ISSN 0360-0327), vol. 12, Nov.-Dec

Astronomy and Astrophysics

Astronomy

11

Binary Stars, Radio Astronomy, Stellar Models, Stellar Spectrophotometry, Accretion Disks, Giant Stars, Light Curve, White Dwarf Stars

Scientific paper

The photometric, spectroscopic and radio-flux observations during the 1984 - 1985 brightness decrease are described. The observational data are explained by use of the binary star model. An explosion of hydrogen-rich accreted matter in the white dwarf component's surface is the reason for the simultaneous decrease of the optical flux and the increase of the radio flux. The outburst became to be bipolar because it had been stopped in the equatorial plane by the thick accretion disk. The radio flux is caused by free-free emission of the outflowing gas. After the inner part of the accretion disk is emptied by the explosion, the outer parts fall down and the optical radiation decreases.

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