  We examine the dynamics of particles around a rotating regular black hole. In
particular we focus on the effects of the characteristic length parameter of
the spinning black hole on the motion of the particles by solving the equation
of orbital motion. We have found that there is a fourth constant of motion that
determines the dynamics of orbits out the equatorial plane similar as in the
Kerr black hole. Through detailed analyses of the corresponding effective
potentials for massive particles the possible orbits are numerically simulated.
A comparison with the trajectories in a Kerr spacetime shows that the
differences appear when the black holes rotate slowly for large values of the
characteristic length parameter.
