论文标题
V533 Herculis中永久性超烟的特征
Characteristics of the Permanent Superhumps in V533 Herculis
论文作者
论文摘要
我们分析了Nova样灾难性变量恒星V533 HE的两个领域。我们检测到与二元轨道时期一致的周期性，并估计修订值为3.53709（2）小时。我们还检测到一个强烈的信号在3.8 h的周期接近，我们与正峰缔合。超级频率在苔丝观测值的情况下变化，超级和轨道周期之间的分数差异，$ε$，范围在$ 0.055 \leε\ le 0.080 $之间。超级振幅与其频率相关，使得幅度随着$ε$的减少而增加。积极的超烟是由于产生偏心积聚磁盘和$ε$的不稳定性而产生的，这是衡量二进制休息帧中磁盘进动率的量度。观察到的相关性意味着，随着磁盘进动率的减慢，磁盘偏心率会增加。
We analyze two sectors of TESS photometry of the nova-like cataclysmic variable star V533 Her. We detect a periodicity consistent with the binary orbital period and estimate a revised value of 3.53709(2) hr. We also detect a strong signal near a period of 3.8 h that we associate with positive superhumps. The superhump frequency varies over the TESS observations with the fractional difference between the superhump and orbital periods, $ε$, ranging between $0.055\le ε\le 0.080$. The superhump amplitude is correlated with its frequency such that the amplitude increases as $ε$ decreases. Positive superhumps result from an instability that generates an eccentric accretion disk and $ε$ is a measure of the disk precession rate in the binary rest frame. The observed correlation implies that as the disk precession rate slows, the disk eccentricity increases.
