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- W2301758066 abstract "Strongly magnetized stellar objects have magnetospheres characterized by such activitiesthat define the geometry of the inner edge of the disk as well as control the inflow of matterto the NS surface itself. Of all possible components of the surface magnetic field of the central object (neutron star-NS), we have only considered the quadrupole term to investigatewhat ever is going on nearer to the surface of the NS. There is a highly important differenceof the accretion flow in a quadrupolar and dipolar magnetic fields. The dipolar magneticfield will in the end always present a barrier to the accretion flow since the field lines areperpendicular to the plane of the disk, but the quadrupolar magnetic field will in the simplest case lie in the plane of the disk, and thus it will rather channel the accretion flow allthe way down to the stellar equator. This work involves a mathematical treatment of anaccretion disk around a magnetized star. In order to define the disk structure magnetohydrodynamic (MHD) equations are solved in cylindrical coordinates. For the detailed resultsan ordinary differential equation (ODE) derived from the angular momentum equation isnumerically solved. So, both Keplerian and non-Keplerian cases of thin accretion disk aresolved. Further, introductory work on slim disk is included as a part of this work. Theresults of our analysis indicate the existence of two different regions: a super-Keplerian innermost region and a broader sub-Keplerian outer region. The effects of stellar and toroidalmagnetic fields on the variations of viscosity, temperature and density have also been studied. We have identified the nature of the inner portion of an accretion disk. The velocityof the transition varies from corotating magnetospheric boundary to super-Keplerian forlow density inner most portion of accretion disk, that extends from 0:5RM to the peak andthen to sub-Keplerian. Our results are applicable to accreting astrophysical systems such as neutron stars (NSs) and white dwarfs (WDs). It can also explain observational resultsnot yet fully backed with theories." @default.
- W2301758066 created "2016-06-24" @default.
- W2301758066 creator A5053297324 @default.
- W2301758066 date "2014-04-01" @default.
- W2301758066 modified "2023-09-23" @default.
- W2301758066 title "The Dynamics of Accretion Disks around Compact Stars with Complex Magnetic Fields" @default.
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- W2301758066 hasPublicationYear "2014" @default.
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