AI 中文总结
研究静止磁化吸积环面中剪切粘性对非旋转黑洞阴影合成图像的影响，通过广义相对论辐射传输计算获得图像，经分析发现强磁化环面图像差异大，剪切粘性与时空曲率综合效应在特定条件下更明显，对黑洞阴影图像印记适度，动态吸积系统中影响或更显著。
AI 中文摘要
我们研究了静止磁化吸积环面中的剪切粘性对非旋转黑洞阴影合成图像的影响。通过非理想相对论流体动力学的二阶因果理论中的一阶和二阶输运系数，在环面中微扰地引入剪切粘性和时空曲率贡献。通过广义相对论辐射传输计算，在假设热同步辐射发射的情况下，针对广泛的等离子体磁化参数、观测倾角、电子温度规定和粘性参数，获得了230GHz的合成黑洞阴影图像。使用两个归一化指标进行的逐像素比较分析表明，对于强磁化环面，图像差异最大。虽然剪切粘性仅在整体阴影形态上引起微小变化，但其与时空曲率的综合效应在同步辐射发射的局部修改和逐像素通量分布中更为明显。这些效应在较高倾角下变得越来越明显，对于较大的电子温度参数值，粘性和非粘性配置之间的最大亮度差异出现。总体而言，我们的结果表明，剪切粘性和时空曲率对静止厚盘产生的黑洞阴影图像仅留下适度的印记，差异保持在几微焦耳的水平。由于我们的分析仅限于静止环面，然而，剪切粘性的影响在完全动态的吸积系统中可能更为显著。
英文摘要
We study the effect of shear viscosity in stationary magnetized accretion tori on synthetic images of non-rotating black hole shadows. Shear viscosity and spacetime-curvature contributions are introduced perturbatively in the tori through first and second-order transport coefficients within a second-order causal theory of non-ideal relativistic hydrodynamics. Synthetic black hole shadow images at 230\,GHz are obtained via general relativistic radiative transfer computations assuming thermal synchrotron emission and for a wide range of plasma magnetization parameters, viewing inclination angles, electron-temperature prescriptions, and viscosity parameters. A comparative pixel-by-pixel analysis using two normalized metrics shows that the largest image differences occur for strongly magnetized tori. While shear viscosity induces only minor changes in the overall shadow morphology, its combined effects with spacetime curvature are more evident in localized modifications of the synchrotron emission and pixel-wise flux distribution. These effects become increasingly pronounced at higher inclination angles, with the largest brightness differences between viscous and non-viscous configurations occurring for larger values of the electron-temperature parameter. Overall, our results indicate that shear viscosity and spacetime curvature leave only modest imprints on black hole shadow images produced by stationary thick disks, with differences remaining at the level of a few $μ$Jy. Since our analysis is limited to stationary tori, the effects of shear viscosity might however be more significant in fully dynamical accretion systems.
Comments12 pages, 7 figures
