The Contribbution Of Coulombic Pressure To The Stability Of Thin Keplerian Accretion Discs Around A Neutron Star With Axisymmetric Magnetic Dipole

Based on the contribution of intraction between various charged componentsrnof the system the stability analysis of an axisymmetric geometrically thin andrnoptically thick accretion disk around a magnetized neutron star is presented.Therndisk we consider is modi ed by including the e ect of coulombic pressure on therntotal pressure.We consider three region of the disks outer, middle and inner region.rnThe outer and middle region of the disk is dominated by gas pressure andrnthe inner region is dominated by radiation pressure. The opacity in the middlernand inner region is mainly due to electron scattering whereas that in the outerrnregion is mainly due to free-free emission. Starting from the vertically integratedrnnon-relativistic hydrodynamics equations we set up the basic equations which governrnthe structure of the disc and for the stability analysis of the disc model wernhave kept the time dependencies in the equations. Even if we include coulombicrnpressure We nd that the gas pressure dominated region is thermally stable.Therngraph of stability parameter as afunction of the disk radius shows that the innerrnregion of the disc is viscously unstable

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