Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
Volume 60, Issue 5, Pages 1151-1158Publisher
OXFORD UNIV PRESS
DOI: 10.1093/pasj/60.5.1151
Keywords
accretion, accretion disks; stars: dwarf novae; stars: individual (EG Aquarii); stars: novae, cataclysmic variables; stars: oscillations
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We report on time-resolved CCD photometry of the cataclysmic variable EG Aquarii during a 2006 November outburst. During the outburst, superhumps were unambiguously detected with a mean period of 0.078828(6) d, allowing for the first time to classify the object as an SU UMa-type dwarf nova. It also turned out that the outburst contained a precursor. At the end of the precursor, immature profiles of humps were observed. By a phase analysis of these humps, we interpreted the features as being superhumps. This is the second example that the superhumps were shown during a precursor. Near the maximum stage of the outburst, we discovered an abrupt shift of the superhump period by similar to 0.002d. After the supermaximum, the superhump period decreased at a rate of (P) over dot/P -8.2 x 10(-5), which is typical for SU UMa-type dwarf novae. Although the outburst light curve was characteristic of SU UMa-type dwarf novae, long-term monitoring of the variable shows no outbursts over the past decade. We also comment on the basic properties of long period and inactive SU UMa-type dwarf novae.
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