VZ性别：X射线证实其中间极性
VZ Sex: X-ray confirmation of its intermediate polar nature
摘要：
中间极星是激变变星双星的成员。它们的特征是一颗中等磁化的白矮星从一颗冷的主序星伴星吸积物质。在许多情况下，这种吸积会产生可探测到的PDMATHAMM射线辐射. VZ Sex是一个有趣的$X$射线源，其性质需要一个强有力的证实。在这里，我们使用档案$XMM$ -牛顿观测将源分配到中间极类。我们应用Lomb Scargle周期图方法检测任何相关的周期性特征的$0.1$ - $10$千电子伏光变曲线，并进行光谱拟合的$X$射线光谱，以获得信息的持续吸积机制。通过检查周期图，我们在$\simeq 20.3$分钟处检测到一个清晰的周期性特征，我们将其解释为白矮星的自旋周期。我们还发现了典型的边带预期的结果之间的节拍旋转和轨道周期$\simeq 3.581$小时。该源的特征在于未吸收通量为$\simeq 2.98\times 10^{-12}$ erg cm $^{-2}$ s $^{-1}$，对应于固有光度{对于$\simeq 433$ pc}为$\simeq 7 \times 10^{31}$ erg s $^{-1}$}。这些特征的存在使我们能够将VZ性别分类为中间极性类的明确成员。此外，利用估计的WD自旋，比率$P_{spin}/P_{orb}$为$\simeq 0.09$，即，与对于周期间隙以上的典型IP系统所预期的一致。此外，估计的内在光度打开了一个桥梁的可能性，连接正常明亮的IP的微弱人口的来源确实存在。
英文摘要：
Intermediate polars are members of the cataclysmic variable binary stars. They are characterized by a moderately magnetized white dwarf accreting matter from a cool main-sequence companion star. In many cases, this accretion gives rise to a detectable $X$-ray emission. VZ Sex is an interesting $X$-ray source whose nature needs a robust confirmation. Here, we used archive $XMM$-Newton observation to assign the source to the intermediate polar class. We applied the Lomb-Scargle periodogram method to detect any relevant periodic feature in the $0.1$--$10$ keV light curve and performed a spectral fitting of the $X$-ray spectrum in order to get information on the on-going accretion mechanism. By inspecting the periodogram, we detected a clear periodic feature at $\simeq 20.3$ minutes that we interpret as the spin period of the white dwarf. We additionally found the typical side bands expected as the consequence of the beat between the spin and the orbital period of $\simeq 3.581$ hours. The source is characterized by a unabsorbed flux of $\simeq 2.98\times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$ corresponding to an intrinsic luminosity {of $\simeq 7 \times 10^{31}$ erg s$^{-1}$ } {for a distance of $\simeq 433$ pc}. The existence of such features allow us to classify VZ Sex as a clear member of the intermediate polar class. Furthermore, with the estimated WD spin, the ratio $P_{spin}/P_{orb}$ is $\simeq 0.09$, i.e. consistent with that expected for a typical IP system above the period gap. In addition, the estimated intrinsic luminosity opens the possibility that a bridge linking the normally bright IPs to the faint population of sources does exist.
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