SDSS J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova with Multiple Rebrightenings
SDSS J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova with Multiple Rebrightenings
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DOI：
10.1093/pasj/61.3.601
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发表时间：
2009-03
影响因子：
2.3
通讯作者：
Taichi Kato;E. Pavlenko;H. Maehara;K. Nakajima;M. Andreev;S. Shugarov;P. D. Ponthière;S. Brady;G. Klingenberg;J. Shears;A. Imada
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作者：
Taichi Kato;E. Pavlenko;H. Maehara;K. Nakajima;M. Andreev;S. Shugarov;P. D. Ponthière;S. Brady;G. Klingenberg;J. Shears;A. Imada
我们观测了2006年SDSS J080434.20+510349.2的超级爆发，在其平台期，再增亮阶段，和后超级爆发最终下降。我们发现该天体是一个周期为0.0590048（2）d的掠食系统。只有在超级爆发高原的晚期才能观测到清晰的食，在随后的阶段，食的深度逐渐减小。我们确定了超爆发平台期的超峰周期为0.059539（11）d，给出了0.90（2）%的部分超峰超出。在再亮阶段和超爆发后阶段，持续的超峰比平台阶段的超峰具有更长的周期：在再亮阶段为0.059632（6）d，在最终衰退阶段为0.05969（4）d。这一现象与先前已知的GW Lib、V455 And和WZ Sge中的长周期“晚期超级峰”非常一致。不同再亮状态之间的轨道峰的振幅表明，这些峰不是由经典热点产生的，而更可能是高倾角系统中投影效应的结果。没有明确的证据表明在再亮阶段有一个增强的热点。我们还研究了以前报道的“迷你爆发”在静止状态下，并发现证据表明，超级驼峰在这些迷你爆发瞬态激发。SDSS J080434.20+510349.2中掠食和明显的多次再亮现象的存在为理解WZ Sge型矮新星的再亮机制提供了一个独特的机会。
We observed the 2006 superoutburst of SDSS J080434.20+510349.2 during its plateau phase, rebrightening phase, and post-superoutburst final decline. We found that this object is a grazing eclipsing system with a period of 0.0590048(2) d. Well-defined eclipses were only observed during the late stage of the superoutburst plateau and the depth decreased during the subsequent stages. We determined the superhump period during the superoutburst plateau to be 0.059539(11) d, giving a fractional superhump excess of 0.90(2)%. During the rebrightening and post-superoutburst phases, persisting superhumps have periods longer than those of superhumps during the plateau phase: 0.059632(6) d during the rebrightening phase and 0.05969(4) d during the final fading. This phenomenon is very well in line with the previously known long-period “late superhumps” in GW Lib, V455 And, and WZ Sge. The amplitudes of orbital humps between different states of rebrightenings suggest that these humps do not arise from the classical hot spot, but are more likely to be a result of projection effect in a high-inclination system. There was no clear evidence for an enhanced hot spot during the rebrightening phase. We also studied previously reported “mini-outbursts” in the quiescent state, and found evidence that superhumps were transiently excited during these mini-outbursts. The presence of grazing eclipses and distinct multiple rebrightenings in SDSS J080434.20+510349.2 would provide a unique opportunity for understanding the mechanism of rebrightenings in WZ Sge-type dwarf novae.