  We supplement the analytic solution obtained by Matthews O. M., et. al.,
2005, MNRAS, \textbf{356}, 66 to investigate the steady-state structure of
radiation pressure dominated disc under the influence of a stellar magnetic
field which deploys a torque. The solutions converge to the non-magnetic
Shakura N. I., Sunyaev R. A., 1973, A\& A, \textbf{24}, 337 form when magnetic
field of the star tends to zero and also at large radii. Effects of varying the
mass accretion rates and the spin period of a typical neutron star on the disc
parameters are presented. We further report that the presence of a magnetic
correction term $k$ reduces the radial extent upto which radiation pressure and
electron scattering continue to be the major source of pressure and opacity
respectively. We also report that magnetic effects amplify the viscous
timescale several times in the inner disc.
