There is a special interest to understand the dynamical properties of the accretion disk created around the newly formed black hole due to the supermassive black hole binaries which merge inside the gaseous disk. The newly formed black hole would have a kick velocity at up to thousands of km/s that drives a perturbation on a newly accreted torus around the black hole. Some of the observed supermassive black holes at the center of the Active Galactic Nucleus (AGN) move with a certain velocity relative to its broader accretion disk. In this paper, the effects of the kicked black holes onto the infinitesimally thin accreted torus are studied by using the general relativistic hydrodynamical code, focusing on changing the dynamics of the accretion disk during the accretion disk-black hole interaction. We have found the non-axisymmetric global mode m=1 inhomogeneity, which causes a spiral-wave structure, is excited on the torus due to kicked black hole. The higher the perturbation velocity produced by the kicked black hole, the longer time the torus takes to reach the saturation point. The created spiral density waves which rapidly evolve into the spiral shocks are also observed from the numerical simulations. The spiral shock is responsible for accreting matter toward the black hole. Firstly, the spiral-wave structure is developed and the accretion through the spiral arms is stopped around the black hole. At the later time of simulation, the formed spiral shocks partly cause the angular momentum loss across the torus.
Twisted doughnuts: Thick disk torus around equatorial asymmetric black hole
RIKEN iTHEMS（理化学研究所 iTHEMS）；Center of Applied Space Technology and Microgravity (ZARM), University of Bremen（不来梅大学应用空间技术与微重力中心（ZARM））；Gauss-Olbers Space Technology Transfer Center, University of Bremen（不来梅大学高斯-奥尔伯斯空间技术转移中心）；Leibniz University of Hannover（汉诺威莱布尼茨大学）
