Discovery of a New SU UMa-Type Dwarf Nova, V 1028 Cygni
Discovery of a New SU UMa-Type Dwarf Nova, V 1028 Cygni
复制标题
发现新的 SU UMa 型矮新星 V 1028 Cygni
DOI：
--
复制
发表时间：
1996
期刊：
影响因子：
--
通讯作者：
R. Hirata
中科院分区：
文献类型：
--
作者：
Taichi Kato;D. Nogami;S. Masuda;R. Hirata
对天鹅座V10281995年7月爆发的K波段高速CCD测光结果表明，爆发初期存在驼峰结构。我们得到了0.06154（±0.00002）d作为超级峰周期的最佳估计值。我们确认这颗矮新星属于SU Uma恒星。超级爆发后发生了再增亮，可能与正常爆发有关。对超级峰最大值的时间的分析显示了超级峰周期（Pdot =P/P）增加7.54 × 10 - 6的明显证据。只有几颗星（AL Com，T Leo，SW Uma等）有报道说超级峰期会有这样的增长。在超级爆发结束时，我们检测到超级峰的振幅显著增加。这两种性质都不是普通SU Uma星的典型特征。简要讨论了WZ Sge型和SU UMa型矮新星之间的联系。
K-band high-speed CCD photometry of V 1028 Cyg revealed that hump structures existed in the early stage of its 1995 July outburst. We obtained 0.06154 (±0.00002) d as the best estimated period of superhumps. We confirmed that this dwarf nova belongs to the SU UMa stars. A re-brightening occurred after the superoutburst, and may be associated with a normal outburst. An analysis of the timings of superhump maxima showed clear evidence for an increase of the superhump period (Pdot =P/P) with 7.54 x 10~6. Only a few stars (AL Com, T Leo, SW UMa, etc.) are reported to have such an increase of the superhump period. At the end of the superoutburst, we detected that the amplitude of the superhumps increased considerably. Both of these properties are not typical features of ordinary SU UMa stars. The connection between the WZ Sge-type and the SU UMa-type dwarf novae is briefly discussed.