GR-MHD在高能天体物理中的应用
Aspects of GR-MHD in High-Energy Astrophysics
摘要：
本文主要研究广义相对论-磁流体力学在高能天体物理中的应用。我们讨论的相关性的GR-HD同行制定探索几何厚盘模型和约束的GR-MHD塑造吸积配置的物理。描述了围绕中心超大质量黑洞（SMBH）的环面团模型。这些轨道环聚集体形成几何厚，压力支持，完美的流体环，与复杂的不稳定性过程，包括环碰撞出现和授权的范围广泛的活动相关的expectandly嵌入物质环境的活动星系核。一些注释包括在与原喷流相结合的聚集体上，由与几何厚环面相关联的开尖解表示。对GR-MHD公式在高能天体物理学中应用的一些关键概念的探索，首先讨论了最一般的Einstein-Euler-Maxwell系统的初始数据问题，并在相对论几何背景下解决了这个问题。然后将该系统设为拟线性双曲形式，并讨论了降阶过程。然后，考虑确定的对称性的自引力系统的稳定性问题的分析，考虑的几何部分的扰动也准线性双曲发病。因此，我们专注于理想的GR-MHD和自引力等离子体球。最后，我们得出了几何厚GR-HD盘在其GR-HD公式中围绕Kerr SMBH引力的模型，并在盘的力平衡方程中包括环形磁场的影响，确定了其在环面拓扑和稳定性中的影响
英文摘要：
This work focuses on some key aspects of the General Relativistic (GR)-magnetohydrodynamic (MHD) applications in High-Energy Astrophysics. We discuss the relevance of the GR-HD counterparts formulation exploring the geometrically thick disk models and constraints of the GR-MHD shaping the physics of accreting configurations. Models of clusters of tori orbiting a central super-massive black hole (SMBH) are described. These orbiting tori aggregates form sets of geometrically thick, pressure supported, perfect fluid tori, associated to complex instability processes including tori collision emergence and empowering a wide range of activities related expectantly to the embedding matter environment of Active Galaxy Nuclei. Some notes are included on aggregates combined with proto-jets, represented by open cusped solutions associated to the geometrically thick tori. This exploration of some key concepts of the GR-MHD formulation in its applications to High-Energy Astrophysics starts with the discussion of the initial data problem for a most general Einstein-Euler-Maxwell system addressing the problem with a relativistic geometric background. The system is then set in quasi linear hyperbolic form, and the reduction procedure is argumented. Then, considerations follow on the analysis of the stability problem for self-gravitating systems with determined symmetries considering the perturbations also of the geometry part on the quasi linear hyperbolic onset. Thus we focus on the ideal GR-MHD and self-gravitating plasma ball. We conclude with the models of geometrically thick GR-HD disks gravitating around a Kerr SMBH in their GR-HD formulation and including in the force balance equation of the disks the influence of a toroidal magnetic field, determining its impact in tori topology and stability
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