论文标题
三个su uma型矮人的瞬态行为； AR PIC，QW SER和V521 PEG
Transient behavior of three SU UMa-type dwarf novae; AR Pic, QW Ser and V521 Peg
论文作者
论文摘要
其他研究已经检测到了某些Su Uma型矮人Novae的超级周期长度的变化，并表明质量转移率随着时间的推移明显降低。我们研究了三个Su Uma型矮人Novae的超级循环长度：AR PIC，QW SER和V521 PEG，以确定它们是否在超级环境中有可检测的变化。我们介绍了这些来源的光谱和光度观察结果。我们的观察结果于2016年和2017年在南非天文天文台的博伊登天文台和萨瑟兰站进行。静止的结果表明，这三个来源都是典型的su uma型矮人。我们还在前体爆发和Superoutburst期间介绍了AR PIC和QW SER的结果。光曲线是由Catalina实时瞬态调查，ASA-3和ASAS-SN档案以及AAVSO国际数据库补充的光曲线，以研究这些来源的长期行为。我们的结果结合了所有短期矮人Novae的分类性能，显示了SU UMA系统中的超循环时间与它们的轨道周期之间的可能关系，这被解释为随着系统朝着“周期最小值”的发展和远距离的发展，这被解释为质量转移率的下降。在最短的轨道时期，SU UMA系统几乎与WZ SGE系统无法区分。但是，我们建议，次级光球和L1之间的比例可能是区分Su uma子类的因素。
Changes in the supercycle lengths of some SU UMa-type dwarf novae have been detected by other studies, and indicate that the mass transfer rates noticeably decrease over time. We investigated the supercycle lengths of three SU UMa-type dwarf novae: AR Pic, QW Ser and V521 Peg, to determine if they have detectable changes in their supercycles. We present the results of optical spectroscopic and photometric observations of these sources. Our observations were conducted in 2016 and 2017 at the Boyden Observatory and the Sutherland station of the South African Astronomical Observatory. The quiescent results indicated that all three sources are typical SU UMa-type dwarf novae. We also present results of AR Pic and QW Ser in outburst and of V521 Peg during a precursor outburst and superoutburst. Light curves were supplemented by the Catalina Real-Time Transient Survey, the ASAS-3 and ASAS-SN archives, and the AAVSO International database in order to investigate the long-term behavior of these sources. Our results combined with catalogued properties for all short-period dwarf novae, shows a possible relationship between the supercycle time in SU UMa systems and their orbital periods, which is interpreted as the decline in the mass transfer rate as systems evolve toward and away from the 'period minimum'. At the shortest orbital periods, SU UMa systems are almost indistinguishable from WZ Sge systems. However, we propose that the scaleheight between the secondary's photosphere and L1 may be a factor that distinguish the SU UMa subclasses.
