XMM-Newton observations of the peculiar cataclysmic variable Lanning 386: X-ray evidence for a magnetic primary
XMM-Newton observations of the peculiar cataclysmic variable Lanning 386: X-ray evidence for a magnetic primary
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DOI：
10.1093/mnras/stw3282
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发表时间：
2016-12
影响因子：
4.8
通讯作者：
Mark Kennedy;Mark Kennedy;P. Callanan;P. Garnavich;M. Fausnaugh;J. C. Zinn
中科院分区：
文献类型：
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作者：
Mark Kennedy;Mark Kennedy;P. Callanan;P. Garnavich;M. Fausnaugh;J. C. Zinn
我们提出了对食变星lanning386和MASTER OTJ192328.22+612413.5的第一次x射线观测，它们可能是SW Sextantis系统。Lanning 386的x射线光曲线显示出深日食，与光学光曲线上看到的日食相似，证实了系统的高倾角。朗宁386的x射线光曲线和光学光曲线在17-22 min之间存在周期性，这与准周期振荡有关。该系统还显示了硬x射线光谱，这与部分覆盖、吸收的2温度等离子体很好地吻合。冷等离子体温度（0.24$^{+0.17}_{-0.08}$ keV）和热等离子体温度（9$^{+4}_{-2}$ keV）不是已知中极系统的非典型等离子体温度。基于这个模型，我们认为Lanning 386是一个具有高吸积率的中间极。炽热的等离子体温度将白矮星的质量限制在$>$0.5 M$ {\odot}$。利用大型双筒望远镜获得的光谱，我们发现该系统中的副星与一颗M5V星一致，并将其与Lanning 386的距离细化为160$\pm$50 pc。最后，利用光谱的高时间分辨率对朗宁386白矮星的磁矩进行了粗略的约束。J1923在观测中未被探测到，但通量的上限与J1923和朗宁386相关。
We present the first X-ray observations of the eclipsing cataclysmic variables Lanning 386 and MASTER OTJ192328.22+612413.5, possible SW Sextantis systems. The X-ray light curve of Lanning 386 shows deep eclipses, similar to the eclipses seen in the optical light curve, confirming the high inclination of the system. There is evidence of a periodicity between 17-22 min in the X-ray and optical light curves of Lanning 386, which is associated with quasi-periodic oscillations. This system also displays a hard X-ray spectrum which is well fit by a partially covered, absorbed 2 temperature plasma. The cool plasma temperature (0.24$^{+0.17}_{-0.08}$ keV) and hot plasma temperature (9$^{+4}_{-2}$ keV) are not atypical plasma temperatures of known intermediate polar systems. Based on this model, we suggest that Lanning 386 is an intermediate polar with a high accretion rate. The hot plasma temperature limits the white dwarf mass to $>$0.5 M$_{\odot}$. From the optical spectrum obtained using the Large Binocular Telescope, we find that the secondary in the system is consistent with an M5V star, and refine the distance to Lanning 386 to be 160$\pm$50 pc. Finally, we use the high time resolution of the optical spectra to crudely constrain the magnetic moment of the white dwarf in Lanning 386. J1923 was not detected during the observations, but the upper limit on the flux is inline with J1923 and Lanning 386 being related.