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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >SDSS J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova with Multiple Rebrightenings
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SDSS J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova with Multiple Rebrightenings

机译：SDSS J080434.20 + 510349.2：消除WZ Sge型矮新星并多次增亮

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摘要

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 super-outburst plateau to be 0.059539(11)d, giving a fractional superhump excess of 0.90(2)%. During the rebright_ening 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 rebright_enings in WZ Sge-type dwarf novae.
机译：我们在SDSS J080434.20 + 510349.2的平稳期，增亮阶段和超爆发后的最终下降期间观察到2006年的超爆发。我们发现该对象是周期为0.0590048（2）d的放牧食蚀系统。定义明确的日食仅在超爆发高原的后期才观察到，深度在随后的阶段降低。我们确定超级爆发高原期间的超级驼峰期为0.059539（11）d，给出的超级驼峰分数超过0.90（2）％。在增亮阶段和超爆发后阶段，持续的超级峰的周期比高原阶段的超级峰的周期长：在增亮阶段为0.059632（6）d，在最终衰落阶段为0.05969（4）d。这种现象与GW Lib，V455 And和WZ Sge中先前已知的长期“后期超级驼峰”非常吻合。在不同的增亮状态之间的轨道驼峰的幅度表明，这些驼峰不是由经典热点引起的，而是更有可能是由高倾角系统中的投影效应引起的。没有明显的证据表明在增亮阶段热点增加了。我们还研究了先前报道的处于静止状态的“小爆发”，并发现有证据表明在这些小爆发期间，超级驼峰被瞬间激发。 SDSS J080434.20 + 510349.2中存在掠食和明显的多次增亮，将为了解WZ Sge型矮新星的增亮机理提供独特的机会。

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