Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9+062814

Details Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9+062814 Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9+062814

Aug 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pasj...54..599u&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.54, No.4, pp.599-607

Astronomy and Astrophysics

Astronomy

31

Accretion, Accretion Disks, Stars: Binaries: Close, Stars: Individual (1Rxs J232953.9+062814)

Scientific paper

We report on the evolution of superhumps and late superhumps in an ultrashort period dwarf nova, 1RXS J232953.9 + 062814, during the superoutburst in 2001 November. Ordinary superhumps were observed throughout a plateau phase, a rapid fading phase, and a rebrightening phase. During the plateau phase, the superhump period increased with time at a large rate of Pdot = 1.19 +/- 0.24 × 10-4. In conjunction with the rebrightening phenomenon, these characteristics indicate that an accretion disk expanded further outward from the 3 : 1 resonance radius, which caused a large amount of left over matter at the outer disk, even after the superoutburst. In the post-outburst phase, we detected late superhumps superimposed on dominant double-peak modulations. Late superhumps were observed at least for 10d without a significant period change. We detected the first normal outburst of this object on 2001 December 26. The interval between the super outburst and this normal one is 53d. This short recurrence time supports a high mass-transfer rate in this system. Concerning the evolutionary status of 1RXS J232953.9 + 062814, we propose that it is a progenitor of AM CVn stars on the evolutionary course of the cataclysmic variable channel in which systems have a secondary star with a hydrogen-exhausted core.

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