SDSS J080434 .20+510349.2：见证不稳定带的灾变变量？
SDSS J080434.20+510349.2: Cataclysmic Variable Witnessing the Instability Strip?
摘要：
SDSS J 080434.20 +510349.2是第13颗包含脉动白矮星的矮新星。在经历过矮新星爆发的吸积型超新星中，SDSS J 0804在短时间内有着最戏剧性的事件历史：2006年爆发11次再亮，2006年12月至2007年1月的一系列小型爆发，2010年爆发6次再亮。在2006-2011年期间，SDSS J080434.20+510349.2除了爆发和爆发后1个月的正0.060^d超峰和平静期的0.059005^d轨道峰外，还表现出显著的短期变化，周期P1 = 12.6min，P2 = 21.7min，P3 = 14.1 min，P4 = 4.28 min。12.6 min的周期性在2006年爆发后7个月首次出现，在随后的\sim 900天中最为突出。它被确认为白矮星的非径向脉动。这些脉动的周期在36 s范围内变化，振幅在0.013 ~ 0.03 m之间变化。同时，可以观察到21.7分钟和14.3分钟的周期，显著性水平低得多。在小爆发期间，21.7分钟的周期性变得最强大，12.6分钟的周期性较弱，12.6分钟的周期性具有最低的显著性。2011年爆发后，最突出的短期周期出现\sim爆发后7个月，但在4.28分钟。我们确定，周期P2，P3和P4的变化可能是额外的脉动模式，但P4的关系，白矮星脉动也不能排除。
英文摘要：
SDSS J080434.20+510349.2 is the 13th dwarf nova containing a pulsating white dwarf. Among the accreting pulsators that have experienced a dwarf novae outburst, SDSS J0804 has the most dramatic history of events within a short time scale: the 2006 outburst with 11 rebrightenings, series of December 2006 - January 2007 mini-outbursts, the 2010 outburst with 6 rebrightenings. Over 2006-2011, SDSS J080434.20+510349.2 in addition to positive 0.060^d superhumps during the outburst and 1-month post-outburst stage, 0.059005^d orbital humps in quiescence, displayed a significant short-term variations with periods P1 = 12.6 min, P2 = 21.7 min, P3 = 14.1 min and P4 = 4.28 min. The 12.6-min periodicity first appeared 7 months after the 2006 outburst and was the most prominent one during the following \sim 900 days. It was identified as non-radial pulsations of the white dwarf. The period of this pulsations varied within a range of 36 s, and amplitude changed from 0.013m to 0.03m. Simultaneously one could observe the 21.7-min and 14.3-min periodicities with a much lower significance level. During the minioutbursts the 21.7-min periodicity became the most powerful, the 12.6-min periodicity was less powerful, and the 12.6-min periodicity had the lowest significance. After the 2011 outburst the most prominent short-term periodicity appeared \sim 7 months after the outburst, but at 4.28 min. We identified that variability with periods P2, P3 and P4 could be additional pulsation modes, however the relation of P4 to white dwarf pulsation also can't be excluded.
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