Dwarf novae: Observational results and their interpretation. I - Light variations; basic model of a cataclysmic binary; outburst models

Details Dwarf novae: Observational results and their interpretation. I - Light variations; basic model of a cataclysmic binary; outburst models Dwarf novae: Observational results and their interpretation. I - Light variations; basic model of a cataclysmic binary; outburst models

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983s%26w....22..123v&link_type=abstract

Sterne und Weltraum, vol. 22, Mar. 1983, p. 123-128. In German.

Astronomy and Astrophysics

Astronomy

Astronomical Photometry, Binary Stars, Dwarf Novae, Stellar Models, Light Curve, Mass Transfer, Stellar Spectra

Scientific paper

The first 'dwarf nova', the U Gem, was discovered by Hind in 1855. A 'dwarf nova' represents a special type of variable star. Such a variable is in most cases a very faint star which becomes suddenly much brighter. After retaining the maximum brightness for a few days, the star becomes gradually fainter until its minimum brightness level is reached again. The sudden increase in the brightness level of the star occurs generally at intervals of approximately 100 days. However, there are cases in which the repetition rates for the maxima are quite different. Spectroscopic investigations have shown that dwarf novae are spectroscopic binaries. They belong to the category of cataclysmic binaries. The primary component of the binary is a white dwarf, while the secondary component is a cool main sequence star. The basic model of a cataclysmic binary is discussed in detail along with two possibilities regarding the physical basis of the outbursts.

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