The SU UMa Nature of the Dwarf Nova, DM Lyrae
The SU UMa Nature of the Dwarf Nova, DM Lyrae
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矮新星的 SU UMa 本质，DM Lyrae
DOI：
10.1093/pasj/55.2.483
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发表时间：
2003
影响因子：
2.3
通讯作者：
T. Kato
中科院分区：
文献类型：
--
作者：
D. Nogami;H. Baba;K. Matsumoto;T. Kato
我们在1996年7月和1996年2-3月在京都大学的Ouda站和大阪京都大学进行了长时间爆发期间DM LYR的时间分辨V波段光度测量。由于在光曲线上有明显的超峰，Dm LYR首次被确认为一颗Su Uma型矮新星。超峰期为0.0673(2)d，超峰率为2.8(3)%。超暴的持续时间、爆发幅度、平台期的衰减率和超峰超额是一颗常见的苏乌玛星的典型数值。根据向VSNET报告的视觉和CCD观测，这颗恒星经历了爆发模式的戏剧性变化，从超级爆发阶段到正常爆发阶段。可能存在减少两次连续超暴之间的正常爆发次数和延长超暴复发周期的机制。
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 atOsaka 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 superoutburstsand to elongate the recurrence cycle of the superoutburst.