In this paper we report on the formation of magnetically-levitating accretion disks around supermassive black holes. The structure of these disks is calculated by numerically modelling tidal disruption of magnetized interstellar gas clouds. We find that the resulting disks are entirely supported by the pressure of the magnetic fields against the component of gravitational force directed perpendicular to the disks. The magnetic field shows ordered large-scale geometry that remains stable for the duration of our numerical experiments extending over 10% of the disk lifetime. Strong magnetic pressure allows high accretion rate and inhibits disk fragmentation. This in combination with the repeated feeding of manetized molecular clouds to a supermassive black hole yields a possible solution to the long-standing puzzle of black hole growth in the centres of galaxies.
Synchrotron Self-Absorption Spectral Modeling Reveals a Magnetically Driven Shock-in-Jet Scenario in Blazar 1156+295
State Key Laboratory of Radio Astronomy and Technology, Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台射电天文与技术重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（匈牙利科学院天文与地球科学研究中心孔科利天文台）；CSFK, MTA Centre of Excellence, Konkoly Thege Miklós út 15-17（MTA卓越中心宇宙物理研究所）；State Key Laboratory of Radio Astronomy and Technology, Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台射电天文与技术重点实验室）
Fast X-ray Variability from the Coronae of Supermassive Black Holes
California Institute of Technology（加州理工学院）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Columbia University（哥伦比亚大学）；Clemson University（克莱姆森大学）
An Analytic Model For Magnetically-Dominated Accretion Disks
California Institute of Technology（加州理工学院）；University of Otago（奥塔哥大学）；Princeton University（普林斯顿大学）；University of Toronto（多伦多大学）；Harvard University（哈佛大学）；Flatiron Institute（平坦研究所）；Northwestern University（西北大学）；Wesleyan University（卫斯理安大学）
$\textit{BMAD}$-Circumbinary Magnetically Arrested Disks around Stellar or Black Hole Binaries: Hot Accretion Flows, Disk Properties, and Angular Momentum Transfer
Korea Astronomy and Space Science Institute (KASI)（韩国天文学与空间科学研究所）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）；School of Computer Science and Information Engineering, Changzhou Institute of Technology（常州工学院计算机科学与信息工程学院）；Center for Astronomy and Astrophysics and Department of Physics, Fudan University（复旦大学天文与天体物理中心及物理系）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）；University of Science and Technology（科学技术大学）；Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文系）；School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；College of Physics, Guizhou University（贵州大学物理学院）；Deep Space Exploration Laboratory（深空探索实验室）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；State Key Laboratory of Radio Astronomy and Technology, Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台射电天文与技术国家重点实验室）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）
