Accreting black holes skewing and bending the optical emission from massive Wolf–Rayet companions – a case study of IC10 X-1
Accreting black holes skewing and bending the optical emission from massive Wolf–Rayet companions – a case study of IC10 X-1
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吸积黑洞使大质量沃尔夫-拉叶伴星的光学发射发生倾斜和弯曲——IC10 X-1 的案例研究
DOI：
10.1093/mnras/stad2094
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发表时间：
2023
影响因子：
4.8
通讯作者：
Kazanas, Demosthenes
中科院分区：
文献类型：
--
作者：
Bhattacharya, Sayantan;Christodoulou, Dimitris M.;Chene, André-Nicolas;Laycock, Silas G. T.;Binder, Breanna A.;Kazanas, Demosthenes
我们对高质量 X 射线双星 IC10 X-1 的黑洞和沃尔夫拉叶 (WR) 星光谱中的 Heii4686 发射线进行了统计分析。这条线明显倾斜，三阶矩（倾斜度）随双星轨道相位的变化而变化。我们描述了一种提取仅位于噪声连续体上方的弱/微弱特征的新方法。利用这些特征的矩，我们能够将这些斜线分解为两个对称的高斯分布，作为轨道相位的函数。由于这种双星系统中风与吸积流相互作用的复杂性，这种分解的天体物理学意义非常重大。此前的研究已经表明恒星的径向速度曲线和X射线日食存在0.25的相位滞后，这表明Heiiemitters可能处于恒星风中，因此无法追踪恒星的轨道运动。这项工作的结果进一步表明存在两个独立的发射区域，一个位于 WR 恒星阴影中的星风中，另一个位于影响黑洞外吸积盘的吸积流中；并且观察到的倾斜螺旋线可以通过两个相应的时间相关高斯发射轮廓的叠加来再现。
We present a statistical analysis of the Heii4686 emission line in the spectra of the black hole and Wolf–Rayet (WR) star of the high-mass X-ray binary IC10 X-1. This line is visibly skewed, and the third moment (skewness) varies with the binary’s orbital phase. We describe a new method of extracting such weak/faint features lying barely above a noisy continuum. Using the moments of these features, we have been able to decompose these skewed lines into two symmetric Gaussian profiles as a function of the orbital phase. The astrophysical implications of this decomposition are significant due to the complex nature of wind–accretion stream interactions in such binary systems. Previous studies have already shown a 0.25 phase lag in the radial velocity curve of the star and the X-ray eclipse, which indicates that the Heiiemitters might be in the stellar wind, hence not tracing the star’s orbital motion. Results from this work further suggest the existence of two separate emitting regions, one in the stellar wind in the shadow of the WR star and another in the accretion stream that impacts the black hole’s outer accretion disc; and the observed skewed Heiilines can be reproduced by superposition of the two corresponding time-dependent Gaussian emission profiles.