Dips and eclipses in the X-ray binary Swift J1858.6-0814 observed with NICER
Dips and eclipses in the X-ray binary Swift J1858.6-0814 observed with NICER
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用 NICER 观察到的 X 射线双星 Swift J1858.6-0814 中的倾角和日食
DOI：
10.1093/mnras/stab863
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发表时间：
2021
影响因子：
4.8
通讯作者：
Buisson D
中科院分区：
文献类型：
--
作者：
Buisson D
本文介绍了在X射线双星Swift J1858.6-0814的X射线光变曲线中发现的食。从这些数据中，我们发现轨道周期为s（<$21.3小时），日食持续时间为s（<$1.14小时）。我们还发现在食前阶段的几个吸收下降。由食时与轨道周期之比，可将双星轨道倾角限制在70°以上。伴星质量最可能的范围表明倾角可能比90更接近这个值。日食也与早期的数据一致，其中强烈的变化（“耀斑”）和长的轨道周期阻止了对周期或日食的清晰检测。我们还发现，明亮的耀斑优先发生在日食后阶段的轨道，可能是由于增加的厚度在盘吸积流界面防止耀斑在日食前阶段可见。这支持了变量模糊化是Swift J1858.6-0814中异常强大的可变性的原因。
We present the discovery of eclipses in the X-ray light curves of the X-ray binary Swift J1858.6–0814. From these, we find an orbital period ofs (≈21.3 h) and an eclipse duration ofs (≈1.14 h). We also find several absorption dips during the pre-eclipse phase. From the eclipse duration to orbital period ratio, the inclination of the binary orbit is constrained toi> 70°. The most likely range for the companion mass suggests that the inclination is likely to be closer to this value than 90. The eclipses are also consistent with earlier data, in which strong variability (‘flares’) and the long orbital period prevent clear detection of the period or eclipses. We also find that the bright flares occurred preferentially in the post-eclipse phase of the orbit, likely due to increased thickness at the disc-accretion stream interface preventing flares being visible during the pre-eclipse phase. This supports the notion that variable obscuration is responsible for the unusually strong variability in Swift J1858.6–0814.