In this paper , we present a complete structure of a quasi-Keplerian thin accretion disc with an internal dynamo around a magnetized neutron star .
We assume a full quasi-Keplerian disc with the azimuthal velocity deviating from the Keplerian fashion by a factor \xi~ { } ( 0 < \xi < 2 ) .
In our approach , we vertically integrate the radial component of the momentum equation to obtain the radial pressure gradient equation for a thin quasi-Keplerian accretion disc .
Our results show that at large radial distance the accretion disc behaves in a Keplerian fashion .
But , close to the neutron star , pressure gradient force ( PGF ) largely modifies the disc structure resulting into sudden dynamical changes in the accretion disc .
The corotation radius is shifted inwards ( outwards ) for \xi > 1 ( for \xi < 1 ) and the position of the inner edge with respect to the new corotation radius is also relocated accordingly as compared to the Keplerian model .
The resulting PGF torque couples with viscous torque ( when \xi < 1 ) to provide a spin-down torque and a spin-up torque ( when \xi > 1 ) while in the advective state .
Therefore , neglecting the PGF is a big omission as has been the case in previous models .
This result has the potential of explaining the observable dynamic consequences of accretion discs around magnetized neutron stars .