吸积盘风在黑洞暂现源光学光变谱中留下独特印记
Accretion disc winds imprint distinct signatures in the optical variability spectrum of black hole transients
AI总结：
研究首次将rms光谱方法用于V404 Cygni光学观测，发现吸积盘风导致吸收及反转P-Cygni等独特光变特征。
摘要：
将以均方根（rms）衡量的吸积系统光变性作为能量的函数进行量化，是约束这些天体物理性质的有力工具。本文首次将该方法应用于低质量X射线双星的光学光谱。我们使用Gran Telescopio Canarias（加那利大望远镜）在黑洞暂现源V404 Cygni 2015年爆发期间获取的高时间分辨率数据。在此事件中，流量光谱中检测到了显著的风相关特征，例如P-Cygni轮廓。我们发现，rms光谱包含丰富的光谱特征，尽管其形态通常不同于对应的流量光谱。具体而言，我们通常在流量光谱中发射线所在的位置观测到吸收成分。类似地，在分析光学流量具有显著光变性的片段时，P-Cygni线轮廓在rms光谱中呈现反转（即蓝移区域的光变性增强，同时与红端成分相关的光变性降低）。我们讨论了这些特征的可能起源，它们类似于在活动星系核等其他天体中发现的特征。最后，我们强调该技术在未来搜寻吸积致密天体中的风型外流方面的潜力。
英文摘要：
Quantifying the variability, measured as the root mean square (rms), of accreting systems as a function of energy is a powerful tool for constraining the physical properties of these objects. Here, we present the first application of this method to optical spectra of low-mass X-ray binaries. We use high-time-resolution data of the black hole transient V404 Cygni, obtained with the \textit{Gran Telescopio Canarias} during its 2015 outburst. During this event, conspicuous wind-related features, such as P-Cygni profiles, were detected in the flux spectra. We find that rms spectra are rich in spectral features, although they are typically morphologically different from their flux counterparts. Specifically, we typically observe absorption components in correspondence to the presence of emission lines in the flux spectra. Similarly, when analysing segments with significant variability in the optical flux, P-Cygni line profiles appear inverted in the rms spectra (i.e., enhanced variability in the blue-shifted region, accompanied by a decrease in that associated with the red component). We discuss the possible origin of these features, which resemble those found in other objects, such as active galactic nuclei. Finally, we highlight the potential of this technique for future searches for wind-type outflows in accreting compact objects.
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