  In this paper, we present the complete structure of a quasi-Keplerian thin
accretion disk with an internal dynamo around a magnetized neutron star. We
assume a full quasi-Keplerian disk with the azimuthal velocity deviating from
the Keplerian fashion by a factor of $\xi$ ($0<\xi<2$). 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
disk. Our results show that, at large radial distance, the accretion disk
behaves in a Keplerian fashion. However, close to the neutron star, pressure
gradient force (PGF) largely modifies the disk structure, resulting into sudden
dynamical changes in the accretion disk. The corotation radius is shifted
inward (outward) 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, as has
been the case in previous models, is a glaring omission. Our result has the
potential to explain the observable dynamic consequences of accretion disks
around magnetized neutron stars.
