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arXiv 1003.4996astro-ph.SR
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激变变星中长时标光度变化的SuperWASP观测

SuperWASP observations of long timescale photometric variations in cataclysmic variables

N. L. Thomas, A. J. Norton, D. Pollacco, R. G. West, P. J. Wheatley, B. Enoch, W. I. Clarkson

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13 figures
发表信息：
Astronomy & Astrophysics, 2010
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摘要：

我们研究了Stanishev等人（2002）关于日蚀深度与其逆行盘进动阶段之间可能存在关系的预测和结果是否可以在SuperWASP的长期观测中得到证实。此外，还对同一SuperWASP数据集中的另外两个CV（DQ Her和V795 Her）进行了研究，以确定是否存在超级驼峰周期和盘进动周期的证据，以及可以检测到其他长期周期（如果有的话）。我们对PX_x的周期和食分析结果证实了负超峰周期为0.1417 \pm 0.0001 d。在我们的数据中，我们没有发现正的超级峰的证据，这表明在我们的观测期间，PX和可能处于低状态。我们改进了现有的估计光盘岁差周期，发现它是4.43 \pm 0.05 d。我们的研究结果证实了Stanishev et al（2002）的预测。我们发现，DQ她似乎并没有表现出类似的变化，我们没有发现负超级驼峰或逆行盘进动的证据。我们也没有发现任何证据的积极的超级驼峰或一个dagede盘进动，我们属性的缺乏积极的超级驼峰在DQ她是由于高质量比的CV。然而，我们确实发现了在100天的时间内日食深度调制的证据，这可能与太阳型磁周期有关，从而引起长期的光度变化。对V795 Her的周期图分析发现其可能的正超峰周期为0.1165d，但没有发现轨道周期为0.10826d，盘旋进周期为1.53d。在这里，虽然我们已经发现了一个变化的周期图功率函数在正的超级驼峰期间，在一段时间内，至少120天。

英文摘要：

We investigated whether the predictions and results of Stanishev et al (2002) concerning a possible relationship between eclipse depths in PX And and its retrograde disc precession phase, could be confirmed in long term observations made by SuperWASP. In addition, two further CVs (DQ Her and V795 Her) in the same SuperWASP data set were investigated to see whether evidence of superhump periods and disc precession periods were present and what other, if any, long term periods could be detected. The results of our period and eclipse analysis on PX And confirm that the negative superhump period is 0.1417 \pm 0.0001d. We find no evidence of positive superhumps in our data suggesting that PX And may have been in a low state during our observations. We improve on existing estimates of the disc precession period and find it to be 4.43 \pm 0.05d. Our results confirm the predictions of Stanishev et al (2002). We find that DQ Her does not appear to show a similar variation for we find no evidence of negative superhumps or of a retrograde disc precession. We also find no evidence of positive superhumps or of a prograde disc precession and we attribute the lack of positive superhumps in DQ Her to be due to the high mass ratio of this CV. We do however find evidence for a modulation of the eclipse depth over a period of 100 days which may be linked with solar-type magnetic cycles which give rise to long term photometric variations. The periodogram analysis for V795 Her detected the likely positive superhump period 0.1165d, however, neither the 0.10826d orbital period or the prograde 1.53d disc precession period were seen. Here though we have found a variation in the periodogram power function at the positive superhump period, over a period of at least 120 days.

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