Structure of the accretion disk in the dwarf nova IP Pegasi

Details Structure of the accretion disk in the dwarf nova IP Pegasi Structure of the accretion disk in the dwarf nova IP Pegasi

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pazh...11..696g&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 11, Sept. 1985, p. 696-705) Soviet Astronomy Letters (ISSN 0360-0327), vol. 11, Sept.-O

Astronomy and Astrophysics

Astronomy

Accretion Disks, Dwarf Novae, Flare Stars, Stellar Activity, Stellar Mass Ejection, Ubv Spectra, Light Curve, Stellar Mass Accretion, Stellar Spectrophotometry

Scientific paper

The brightness distribution over the edge-on accretion disc is investigated by means of photoelectric UBV observations of eclipses in the close binary system IP Pegasi. The radiation of a hot spot is predominant. The brightness and location of the spot in the disc change depending on the phase of activity. In a quiet state the disc is surrounded by an extended obscure ring, a small sector of which is shining when the star brightness falls down after the outburst. The observations support the model of a strengthening gas flow from the secondary star to explain the cause of outbursts.

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