The 2003/2004 Superoutburst of SDSS J013701.06-091234.9
The 2003/2004 Superoutburst of SDSS J013701.06-091234.9
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DOI：
10.1093/pasj/58.1.143
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发表时间：
2005-08
影响因子：
2.3
通讯作者：
A. Imada;Taichi Kato;K. Kubota;M. Uemura;R. Ishioka;S. Kiyota;K. Kinugasa;H. Maehara;K. Nakajima;L. Monard;D. Starkey;A. Oksanen;D. Nogami
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作者：
A. Imada;Taichi Kato;K. Kubota;M. Uemura;R. Ishioka;S. Kiyota;K. Kinugasa;H. Maehara;K. Nakajima;L. Monard;D. Starkey;A. Oksanen;D. Nogami
我们报道了在2003年12月至2004年1月期间，一颗SU uma型矮新星SDSS J013701.06−091234.9的超爆发的时间分辨光度测定。获得的光曲线明确地显示出周期为0.056686(12)d的超级峰，这是迄今观测到的SU - uma型矮新星中最短的超级峰周期之一。考虑到静态光度学研究，我们估计分数超驼峰过剩为0.024。Szkody等人（2003，AJ, 126,1499）的光谱观测提供了TiO波段的证据，尽管轨道周期很短，这意味着该系统有一颗明亮的副星。我们利用2MASS档案绘制了SU uma型矮新星静止状态的彩色图，发现这颗恒星在彩色图中的位置偏离了一般趋势。根据经验周期-绝对星等关系，基于固有运动，粗略估计到系统的距离为300±80pc。
We report on time-resolved photometry of the superoutburst of an SU UMa-type dwarf nova, SDSS J013701.06−091234.9, in 2003 December–2004 January. The obtained light curves definitely show superhumps with a period of 0.056686(12)d, which is one of the shortest superhump periods among those of SU UMa-type dwarf novae ever observed. Considering quiescent photometric studies, we estimated the fractional superhump excess to be 0.024. Spectroscopic observations by Szkody et al. (2003, AJ, 126, 1499) provided evidence for TiO bands despite the short orbital period, implying that the system has a luminous secondary star. We have drawn a color–color diagram of SU UMa-type dwarf novae in quiescence using 2MASS archives, revealing that the location of this star in the color-color diagram deviates from the general trend. The distance to the system was roughly estimated to be 300 ±80pc, using the empirical period–absolute magnitude relation and based on the proper motion.