The SU UMa Nature of the Dwarf Nova, DM Lyrae

Abstract

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 with 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 the normal outburst between two successive superoutbursts and to elongate the recurrence cycle of the superoutburst.

6 pages, 5 figures, accepted for publication in PASJ

References in corpus (3)

• The Dwarf Novae of Shortest Period
• Dramatic Changes in the Outburst Properties in V503 Cygni
• Five Dwarf Novae with Orbital Periods Below Two Hours

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• Pulsations, Boundary Layers, and Period Bounce in the Cataclysmic Variable RE J1255+266
• TV Corvi Revisited: Precursor and Superhump Period Derivative Linked to the Disk Instability Model
• Superhumps in the Rarely Outbursting SU UMa-Type Dwarf Nova, HO Delphini
• In-the-Gap SU UMa-Type Dwarf Nova, Var73 Dra with a Supercycle of about 60 Days
• V803 Centauri: Helium Dwarf Nova Mimicking a WZ Sge-Type Superoutburst
• Dramatic Spectral Evolution of WZ Sagittae during the 2001 Superoutburst
• Photometric study of southern SU UMa-type dwarf novae and candidates -- III: NSV 10934, MM Sco, AB Nor, CAL 86
• A New SU UMa-Type Dwarf Nova, QW Serpentis (= TmzV46)
• Detection of Short Fading Episodes in Two Dwarf Novae from VSNET Observations