Pseudo-Newtonion potential for the relativistic accretion disk around rotating central objects having hard surface

Abstract

Here we furnish a pseudo-Newtonion potential for accretion disk modeling around rotating central objects having hard sueface. That means, the potential may be useful to describe the accretion disk around rotating neutron stars and strange stars. The potential can describe the general relativistic effects in accretion disk properly, essentially studying the relativistic hydrodynamics of disk. As our intention lies in understanding the fluid dynamics of the accretion disk around rotating central objects with hard surface, it is necessary to incorporate the rotation of the central object which affects the inner edge of the disk. We derive our potential, starting from the Hartle Thorne metric. The potential can reproduce all the essential properties of general relativity with 10% error at most, for slowly rotating neutron/strange stars.

8 pages, aa.cls style; Accepted for publication in Astronomy and Astrophysics (A&A)

References in corpus (4)

• Description of Pseudo-Newtonian Potential for the Relativistic Accretion Disk around Kerr Black Holes
• Pseudo-Newtonian Potentials to Describe the Temporal Effects on Relativistic Accretion Disks around Rotating Black Holes and Neutron Stars
• Effect of Coriolis force on Accretion Flows around Rotating Compact Object
• Hydrodynamical Study of Advective Accretion flow around Neutron Stars

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