Speaker
Description
We present magnetohydrodynamic simulations of a thin accretion disk around a Reissner–Nordström naked singularity, modeled with our pseudo-Newtonian potential. This potential accurately reproduces the orbital frequency, including the radius at which it reaches a maximum and eventually vanishes. The latter defines the zero-gravity sphere, below which the net force is repulsive. Our results show that matter accumulates around the singularity, with increased density near the zero-gravity sphere, in agreement with analytical solutions from general relativity. The resulting outflow structures are analyzed and compared with those obtained from general relativistic magnetohydrodynamic simulations in order to assess the range of applicability of our pseudo-Newtonian potential.