Quasi-periodic luminosity variations in dwarf novae

Details Quasi-periodic luminosity variations in dwarf novae Quasi-periodic luminosity variations in dwarf novae

Apr 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apjs...39..461r&link_type=abstract

Astrophysical Journal Supplement Series, vol. 39, Apr. 1979, p. 461-480.

Astronomy and Astrophysics

Astrophysics

80

Novae, Periodic Variations, Stellar Luminosity, White Dwarf Stars, X Ray Stars, Eclipsing Binary Stars, Frequency Response, Light Curve, Oscillations, Stellar Mass Accretion

Scientific paper

Quasi-periodic oscillations in the light curves of five dwarf novae, U Gem, SS Cyg, RU Peg, KT Per, and VW Hyi, as well as in the light curve of the X-ray source Sco X-1 are identified. The mean periods of the quasi-periodic oscillations are shown to range from 32 s in SS Cyg to 147 s in KT Per, and 165 s in Sco X-1, with the amplitudes being 0.005-0.01 mag. The length of time over which the quasi-periodic oscillations maintain coherence is observed to be very short, typically 3-5 cycles of the oscillations, indicating that the quasi-periodic oscillations can be distinguished from the short-period coherent oscillations in dwarf novae. It is proposed that the quasi-periodic oscillations of dwarf novae and Sco X-1 are produced by their accretion disks.

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