Largest Black Holes in the SkyOrigin and Evolution of Horizon-Scale Structures

在强大的引力场和磁场的相互作用下，极端条件在宇宙环境中形成。尤其是位于星系核中的快速旋转黑洞的邻近区域。我们建议在空间尺度上研究流入/流出相互作用、潮汐效应和广义相对论(GR)作用于吸积等离子体并导致瞬变激波和随后的粒子加速的过程，这些过程可以与事件视界和相应的动力学时间相媲美。只是现在这些过程可以通过高角分辨率观测技术获得，它们的解释需要理论探索。拟议的合作项目将捷克团队(由布拉格的V.Karas领导)在GR相对论天体物理领域的先前经验，特别是在强重力下气体吸积盘中运行的辐射过程的背景下，与德国团队(由科隆的A.Eockart领导)在银河中心超大质量黑洞(SMBH)观测、建模和数据解释方面的持久经验相结合。在GR框架内，我们将讨论可以加速粒子并从被外部源磁化的SMBHs产生耀斑的天体物理机制。快速旋转(旋转)是我们的场景中的一个基本要素。我们将探索加速物质在磁化SMBH附近运动的动力学性质，即从规则运动到混沌运动的转变和混沌开始的重现特征，包括SMBH自旋的作用。我们将把理论模型与观测结果进行比较，特别是在毫米波段和近红外波段。我们希望将注意力集中在现有技术允许的距离黑洞最近的区域。在观测方面，我们将模拟两个杰出天体的观测可变性和结构信息：人马座A*(银河系的非活动中心)和M87(附近活跃的巨型椭圆星系的核心)。在建立模型的同时，我们计划在红外波段进行补充观测，同时进行射电和X射线观测。我们将集中在事件视界望远镜对SgrA*的观测所能获得的区域，为此我们采用了同步的近红外数据。作为最终目标，我们将讨论旋转磁化SMBH框架内的结构特征和可变性属性。在这些天体中精确测量超大质量黑洞的物理参数的前景现在是现实的，也是最令人兴奋的。在一次广泛的合作中，捷克-德国联合小组计划探索解决黑洞吸积问题的不同方法。

Extreme conditions develop in the cosmic environment by the interplay of strong gravitational and magnetic fields. This is particularly the case of the immediate vicinity of rapidly rotating black holes residing in nuclei of galaxies. We pro- pose to study processes of inflow/outflow interaction, tidal effects, and the frame dragging of General Relativity (GR) acting on accreting plasma and leading to transient shocks and the subsequent particle acceleration on spatial scales comparable with the event horizon and the corresponding dynamical time.Only now these processes become accessible observationally via high-angular resolution observational techniques and their interpretation requires theoretical exploration. The proposed collaboration project connects the prior experience of the Czech team (lead by V. Karas in Prague) in the field of GR relativistic astrophysics, especially in the context of radiation processes operating in gaseous accretion discs in strong gravity, and the lasting experience of the German team (lead by A. Eckart in Cologne) in observation, modelling and data interpretation for the Galactic Center supermassive black hole (SMBH).Within GR framework we will discuss astrophysical mechanisms that can accelerate particles and produce flares from SMBHs magnetized by external sources. Rapid rotation (spin) is an essential ingredient in our scenario. We will explore the dynamical properties of motion of accelerated material in the vicinity of magnetized SMBH, namely, the transition from regular to chaotic motion and the Recurrence Characteristics of chaos onset, including the role of SMBH spin. We will compare theoretical models to observations performed especially in millimeter and near-infrared spectral bands. We want to focus our attention on the region as close to the black hole as allowed by the available techniques.On the side of observations, we will model the observed variability and structural information available for two outstanding objects: Sagittarius A* (the inactive center of the Milky Way), and M87 (the nucleus of the nearby active giant elliptical galaxy). Along with the modelling we plan to carry out supplementary observations at infrared wavelengths in conjunction with radio and X-ray observations. We will concentrate on the regime accessible to Event Horizon Telescope Observations of SgrA* for which we take simultaneous NIR data. As a final goal we will discuss the structural features and variability properties within the rotating magnetized SMBH framework. Prospects for precision measurements of the physical parameters of supermassive black holes in these objects are now realistic, and most exciting. In a broad collaboration the joint Czech-German team plans to explore different approaches to the problem of accreting black holes.