A pseudo-Newtonian simulation of accretion onto a Reissner-Nordstrom naked singularity shows the disk thickening at the maximum of the orbital frequency and pushing matter over the top into a torus near the zero-gravity radius.
Three-dimensional structure of an alpha accretion disk
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abstract
An analytic solution is presented to the three-dimensional problem of steady axisymmetric fluid flow through an accretion disk. The solution has been obtained through a systematic expansion in the small parameter epsilon =H/R (the ratio of disk thickness to its radial dimension) of the equations of viscous hydrodynamics. The equation of state was assumed to be polytropic. For all values alpha< 0.685 of the viscosity parameter, we find significant backflow in the midplane of the disk occuring at all radii larger than a certain value; however, in the inner regions of the disk the fluid always flows toward the accreting object. The region of backflow is separated from the region of inflow by a surface flaring outwards from a circular locus of stagnation points situated in the midplane of the disk.
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Pseudo-Newtonian simulation of a thin accretion disk around a Reissner-Nordstr\"om naked singularity
A pseudo-Newtonian simulation of accretion onto a Reissner-Nordstrom naked singularity shows the disk thickening at the maximum of the orbital frequency and pushing matter over the top into a torus near the zero-gravity radius.