On the origin of the two types of outburst of U GEM stars and the mechanism of occurrence of superhumps

Details On the origin of the two types of outburst of U GEM stars and the mechanism of occurrence of superhumps On the origin of the two types of outburst of U GEM stars and the mechanism of occurrence of superhumps

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983afz....19..291i&link_type=abstract

(Astrofizika, vol. 19, Apr.-June 1983, p. 291-301) Astrophysics (ISSN 0571-7132), vol. 19, no. 2, Oct. 1983, p. 168-175. Transla

Astronomy and Astrophysics

Astrophysics

2

Binary Stars, Bursts, Dwarf Novae, Light Curve, Stellar Radiation, Stellar Models, Stellar Structure

Scientific paper

An analytical model of superhump (Sh) phenomena in the light curves of close binaries of SU UMa type is developed which also explains the origin of the short and long outbursts. Previous models are reviewed and shown not to account for the absence of Shs in short outbursts and the variability of Sh periods. It is proposed that Shs are produced by a compact hot spot situated in the equatorial plane of the rotating cool component, this spot being a region through which energy accumulated in the interior of the star is released for transfer to the hot component, causing the increase in envelope emission observed as an outburst. Compact spots tend to give longer-duration outbursts with observable Shs, while large or multiple spots release their energy in a shorter time with hard-to-observe rotational effects. These principles are examined quantitatively, and the mechanisms of spot formation are considered. Calculations for the typical system VW Hyd give an estimated red-component rotational period of 2.85 days.

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