论文标题
从光谱和Cygnus X-1的定时分析推断出的频谱状态之间的增生模式的演变，并具有Insight-HXMT观测值
Evolution of Accretion Modes between Spectral States Inferred from Spectral and Timing Analysis of Cygnus X-1 with Insight-HXMT observations
论文作者
论文摘要
我们在低/硬，中间和高/软状态下对Cygnus X-1进行了详细的频谱定时研究，并进行了硬X射线调制望远镜观察。宽带的能量光谱与积聚磁盘的内部边界非常适合“截短磁盘模型”，在$ \ sim $ 10 \ textit r $ _ {\ rm g} $中保持在$ \ sim $ 10 \ sim $ \ sim $ \ sim $ \ sim $ 10 \ sim $ 10 \ sims $ _ {\ rm g} $中，并随着源软化而向内移动。通过研究PDS，RMS和傅立叶频率分量分辨光谱法，我们发现X射线变化是在每个状态的两个不同区域生成的。我们发现有助于X射线变化的主要作用是热的电晕，而不是吸积盘。我们建议根据截短的磁盘几何形状，为每个状态提供不同的电晕几何形状的场景，在该几何形状中，电晕包裹磁盘以在低/硬状态下形成三明治几何形状，然后逐渐从磁盘上逐渐从磁盘上移开，该方向垂直于磁盘，直至形成高/柔软状态的喷气样几何形状。
We execute a detailed spectral-timing study of Cygnus X-1 in the low/hard, intermediate and high/soft states with the Hard X-ray Modulation Telescope observations. The broad band energy spectra fit well with the "truncated disk model" with the inner boundary of the accretion disk stays within $\sim$10 \textit R$_{\rm g}$ and moves inward as the source softens. Through studying of PDS, rms and Fourier-frequency component resolved spectroscopy, we find that the X-ray variations are generated in two different regions for each state. We discover that the major role that contributes to the X-ray variation is the hot corona rather than the accretion disk. We suggest a scenario with different corona geometry for each state based on the truncated disk geometry in which the corona wraps up the disk to form a sandwich geometry in the low/hard state, and then gradually moves away from the disk in direction that is perpendicular to the disk until forming a jet-like geometry in the high/soft state.
