在这项工作中，我们提出了三维数值相对论模拟厚吸积盘周围倾斜克尔BH。我们研究了三种不同初始盘模型在一系列初始黑洞自旋幅度和倾斜角下的演化。对于所有考虑的盘-黑洞质量比（0.044 - 0.16），我们观察到显着的黑洞岁差和章动在演化过程中。这表明，对于这样的质量比，通过在固定的背景黑洞时空中演化来忽略盘的自引力是不合理的。我们发现，这两个更大规模的模型是不稳定的Papaloizou-Pringle（PP）的不稳定性，这些PP-不稳定的模型仍然不稳定的所有初始自旋和倾斜角考虑，显示不稳定性的发展是一个非常强大的功能，这样的PP-不稳定磁盘。我们最轻的模型是稳定的，它是天体物理学上最有利的致密双星合并的结果。黑洞自旋和盘之间的倾斜在PP不稳定性的增长过程中被强烈调制，导致在具有恒定比角动量l的最大质量模型中黑洞自旋和盘角动量的部分全局重新排列。对于具有非恒定l轮廓的模型，我们观察到一个长寿命的m = 1非轴对称结构，该结构在盘的内部区域显示出倾角的强烈振荡。这种效应可能与Kozai-Lidov振荡的发展有关。我们的模拟也证实了早期的研究结果，PP不稳定性的发展导致长期发射的大振幅引力波，主要是为l = m = 2多极模式。BH旋进对倾斜BH环面系统的引力波的影响仍然是一个有趣的开放性问题，需要比这项工作中提出的时间长得多的模拟。
英文摘要：
In this work we present 3D numerical relativity simulations of thick accretion disks around tilted Kerr BH. We investigate the evolution of three different initial disk models with a range of initial black hole spin magnitudes and tilt angles. For all the disk-to-black hole mass ratios considered (0.044-0.16) we observe significant black hole precession and nutation during the evolution. This indicates that for such mass ratios, neglecting the self-gravity of the disks by evolving them in a fixed background black hole spacetime is not justified. We find that the two more massive models are unstable against the Papaloizou-Pringle (PP) instability and that those PP-unstable models remain unstable for all initial spins and tilt angles considered, showing that the development of the instability is a very robust feature of such PP-unstable disks. Our lightest model, which is the most astrophysically favorable outcome of mergers of binary compact objects, is stable. The tilt between the black hole spin and the disk is strongly modulated during the growth of the PP instability, causing a partial global realignment of black hole spin and disk angular momentum in the most massive model with constant specific angular momentum l. For the model with non-constant l-profile we observe a long-lived m=1 non-axisymmetric structure which shows strong oscillations of the tilt angle in the inner regions of the disk. This effect might be connected to the development of Kozai-Lidov oscillations. Our simulations also confirm earlier findings that the development of the PP instability causes the long-term emission of large amplitude gravitational waves, predominantly for the l=m=2 multipole mode. The imprint of the BH precession on the gravitational waves from tilted BH-torus systems remains an interesting open issue that would require significantly longer simulations than those presented in this work.
Tilted thin accretion disks in the full Kerr spacetime and their implications
Manipal Centre for Natural Sciences, Manipal Academy of Higher Education（马尼帕尔高等教育局马尼帕尔自然科学中心）；Tata Institute of Fundamental Research（塔塔基础研究所）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）
Reshaping the inner shadow of a Kerr black hole by a torn accretion disk
School of Mathematics and Physics, University of South China（南华大学数学与计算学院）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Department of Mechanics, Chongqing Jiaotong University（重庆交通大学力学系）
Construction of an analytic multi-component accretion environment and its application to Kerr black hole imaging
School of Mathematics and Physics, University of South China（南华大学数学与物理学院）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Department of Mechanics, Chongqing Jiaotong University（重庆交通大学力学系）
Relativistic Thermal Emission from Accretion Disks in Kerr-MOG Spacetimes
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大汤川研究所）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Key Laboratory for Particle Astrophysics and Cosmology (MOE) and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University（粒子天体物理宇宙学教育部重点实验室和上海市粒子物理与宇宙学重点实验室，上海交通大学）；Institut für Theoretische Physik, Goethe-Universität Frankfurt（法兰克福歌德大学理论物理研究所）；Institute for Theoretical Physics & Cosmology, Zhejiang University of Technology（浙江工业大学理论物理与宇宙学研究所）
Imprints of Black Hole Shadows and Polarization Patterns of Various Thick Disks: Bumblebee gravity
University of Management and Technology（管理技术大学）；Princess Nourah bint Abdulrahman University（公主努拉·宾特·阿卜杜勒·拉赫曼大学）；Chongqing Jiaotong University（重庆交通大学）；Chongqing Normal University（重庆师范大学）
Dynamics and Radiative Signatures of Accretion Flows onto a Kerr-like Wormhole
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大李政道研究所）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Key Laboratory for Particle Physics, Astrophysics and Cosmology (MOE), Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai Jiao Tong University（粒子物理、天体物理与宇宙学教育部重点实验室，上海粒子物理与宇宙学重点实验室，上海交通大学）
Optical and thermodynamic properties of Kerr-Bertotti-Robinson black holes
California State University, Fresno（弗雷斯诺加州州立大学）；University of Hradec Králové（赫拉德茨克拉洛韦大学）；Khazar University（卡扎尔大学）；Nazarbayev University（纳扎尔巴耶夫大学）；National Taiwan University（台湾大学）；Arizona State University（亚利桑那州立大学）；University of Helsinki（赫尔辛基大学）；Università di Camerino（卡梅里诺大学）；University at Albany-SUNY（奥尔巴尼纽约州立大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所-布雷拉天文台）；Al-Farabi Kazakh National University（阿尔法拉比哈萨克国立大学）；Center for Theoretical Physics, Khazar University（卡扎尔大学理论物理中心）
