Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
Volume 55, Issue 2, Pages 483-488Publisher
OXFORD UNIV PRESS
DOI: 10.1093/pasj/55.2.483
Keywords
accretion, accretion disks; stars : dwarf novae; stars : individual (DM Lyrae); stars : novae, cataclysmic variables
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We carried out time-resolved V-band photometry of DM Lyr during long outbursts in 1996 July and in 1996 February-March at Ouda Station, Kyoto University, and at Osaka Kyoiku University. Since superhumps were clearly detected in the light curves, DM Lyr was first identified as being an SU UMa-type dwarf nova. The superhump period is 0.0673(2) d. and the superhump excess is 2.8(3)%. The duration of the superoutburst, the outburst amplitude, the decline rate in the plateau phase, and the superhump excess were typical values for a usual SU UMa star. According to visual and CCD observations reported to VSNET, this star has experienced a dramatic change of the outburst pattern from a superoutburst phase to a normal outburst phase. There may exist mechanisms to decrease the number of normal outbursts between two successive superoutbursts and to elongate the recurrence cycle of the superoutburst.
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