共生X射线双星Sct X-1、4U 1700+24和IGR J17329-2731
The Symbiotic X-ray binaries Sct X-1, 4U 1700+24 and IGR J17329-2731
摘要：
共生X射线双星是一个系统的主机中子星吸积形成的风晚型伴星。这些都是罕见的物体，到目前为止，只有少数几个是已知的。共生X射线双星最令人困惑的一个方面是它们可能包含强磁化的中子星。与它们的同伴相比，它们在进化上要年轻得多，因此可能是通过（但鲜为人知的）吸积引起的白矮星坍缩形成的。在本文中，我们进行了宽带X射线和软$γ$射线光谱的两个已知的共生双星，Sct X-1和4U 1700+24，寻找回旋散射功能，可以确认存在强磁化NS的存在。我们利用了可用的Chandra、Swift和NuSTAR数据。我们没有发现任何证据的回旋共振散射功能（CRSF）的情况下，Sct X-1，但在4U 1700+24的情况下，我们建议存在一个可能的CRSF在$\sim$ 16 keV和它的第一谐波在$\sim$ 31 keV，虽然我们不能排除替代的光谱模型的宽带拟合。如果未来的观测证实，4U 1700+24可能是第二个与高磁化吸积体共生的X射线双星。我们还报告了我们对最后发现的共生X射线二进制IGR J17329-2731进行的Swift/XRT的长期监测。监测显示，正如预测的那样，该天体在2017年成为一个持续和可变的来源，显示出持续数日的X射线耀斑和在cluerous风吸积背景下解释的有趣的遮蔽事件。
英文摘要：
Symbiotic X-ray binaries are systems hosting a neutron star accreting form the wind of a late type companion. These are rare objects and so far only a handful of them are known. One of the most puzzling aspects of the symbiotic X-ray binaries is the possibility that they contain strongly magnetized neutron stars. These are expected to be evolutionary much younger compared to their evolved companions and could thus be formed through the (yet poorly known) accretion induced collapse of a white dwarf. In this paper, we perform a broad-band X-ray and soft $γ$-ray spectroscopy of two known symbiotic binaries, Sct X-1 and 4U 1700+24, looking for the presence of cyclotron scattering features that could confirm the presence of strongly magnetized NSs. We exploited available Chandra, Swift, and NuSTAR data. We find no evidence of cyclotron resonant scattering features (CRSFs) in the case of Sct X-1 but in the case of 4U 1700+24 we suggest the presence of a possible CRSF at $\sim$16 keV and its first harmonic at $\sim$31 keV, although we could not exclude alternative spectral models for the broad-band fit. If confirmed by future observations, 4U 1700+24 could be the second symbiotic X-ray binary with a highly magnetized accretor. We also report about our long-term monitoring of the last discovered symbiotic X-ray binary IGR J17329-2731 performed with Swift/XRT. The monitoring revealed that, as predicted, in 2017 this object became a persistent and variable source, showing X-ray flares lasting for a few days and intriguing obscuration events that are interpreted in the context of clumpy wind accretion.
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