Superhumps in Cataclysmic Binaries. XVI. DI Ursae Majoris

Details Superhumps in Cataclysmic Binaries. XVI. DI Ursae Majoris Superhumps in Cataclysmic Binaries. XVI. DI Ursae Majoris

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pasp..111.1275f&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 111, Issue 764, pp. 1275-1280.

Astronomy and Astrophysics

Astronomy

13

Stars: Binaries: Close, Stars: Novae, Cataclysmic Variables, Stars: Individual (Di Ursae Majoris)

Scientific paper

We report photometry of the dwarf nova DI Ursae Majoris during 1997-1998. The star shows an orbital light curve at quiescence with a period of 0.054564(1) days. During superoutburst, it flashes superhumps with a period of 0.05529(5) days. The superhump period excess of 1.3% is quite low among cataclysmic variables, suggesting a weak perturbation on the accretion disk and therefore a secondary of very low mass. But other stars of low period excess are rare eruptors, whereas DI UMa is extremely active with normal outbursts every 8 days and superoutbursts every 30-45 days. This is puzzling. We speculate that the binary really does have a secondary of anomalously low mass but is presently in a high state of a mass-transfer cycle.

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