  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.
