  We have studied shock in magnetized accretion flow/funnel flow in case of
neutron star with bremsstrahlung cooling and cyclotron cooling. All accretion
solutions terminate with a shock close to the neutron star surface, but at some
region of the parameter space, it also harbours a second shock away from the
star surface. We have found that cyclotron cooling is necessary for correct
accretion solutions which match the surface boundary conditions.
