Model of a flare of a U Geminorum-type star

Details Model of a flare of a U Geminorum-type star Model of a flare of a U Geminorum-type star

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pazh....1...23g&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal, vol. 1, Jan. 1975, p. 23-28. In Russian.

Astronomy and Astrophysics

Astronomy

5

Astronomical Models, Binary Stars, Stellar Luminosity, Stellar Mass Ejection, Thermal Instability, Companion Stars, Flares, Stellar Envelopes, White Dwarf Stars

Scientific paper

It is proposed that all phenomena observed during flares of U Gem-type stars may be regarded as consequences of a convectional instability in the companion star. Results of analysis indicate that an increase in the luminosity of the companion is accompanied by a significant increase in the flow of matter onto the disk-like envelope of the primary. The radiation of the disk, and especially of its central region, appears to be predominant during the maximum of brightness. Observational data for SS Cyg, U Gem, and Z Cha are presented as evidence in favor of this hypothesis.

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