  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 that drives a perturbation on a
newly accreted torus around the black hole. In this paper, the effects of the
kicked black holes onto the 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 Papaloizou-Pringle Instability (PPI)
produced 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 funnel walls are also observed from the
numerical simulations. These funnels are responsible for accreting matter
toward the black hole. At the later time of evolution, the accretion through
the funnel is stopped and PPI is developed on the torus around the black hole.
