Geodesic structure of a rotating regular black hole

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.

Automated summary

We investigated the motion of particles around a rotating regular black hole, focusing on the effects of the characteristic length parameter on their dynamics. By solving the equation of orbital motion, we discovered a fourth constant of motion that determines the orbits out of the equatorial plane, similar to the Kerr black hole. Through detailed analysis and numerical simulations, we compared the possible orbits with those in a Kerr spacetime and found differences when the black holes rotate slowly for large characteristic length parameter values.