  We study the time evolution of the entanglement entropy of Hawking radiation
in the $(n+1)-$dimensional Kerr-Newman black hole evaporation by the
holographic approach that considering the $(n+1)-$dimensional AdS eternal black
brane coupled to the auxiliary CFT reservoir is in the Hartle-Hawking state.
The CFT reservoir itself has a holographic dual, the $(n+2)-$dimensional bulk
geometry, and the original $(n+1)-$dimensional AdS-black brane is embedded into
such bulk manifold, which is precisely Randall-Sundrum model.
  According to the island rule [1], the entanglement entropy in semi-classical
gravity can be divided into two parts, one is due to the quantum effects, which
can be obtained by Ryu-Takayanagi conjecture. Another is the gravitational
part, which is equal to the area of the quantum extremal surface divided by
four times the Newton's constant. We show that the entanglement growth in our
holographic system is linear in late times. After Page time, the system reaches
saturation since the entanglement islands appear. In this paper, we will
emphasize how black hole rotation affects entanglement entropy in general
dimensional spacetime.
