  We use Smoothed Particle Hydrodynamics to study viscous accretion flows
around a weakly magnetic neutron star. We show the formation of multiple
``boundary" layers in presence of both cooling and viscosity. We find that with
the introduction of a small viscosity in a sub-Keplerian flow, much like the
wind accretion in HMXBs such as Cir X-1, only a single Normal Boundary Layer
(NBOL) forms to adjust the rotational velocity component. With the increase of
viscosity, the region extends radially and beyond some critical value, a
RAdiative KEplerian Disk/layer (RAKED) forms between the sub-Keplerian flow and
the NBOL. When viscosity is increased further only NBOL and RAKED remain. In
all such cases, the CENtrifugal pressure dominated BOundary Layer (CENBOL) is
formed, away from the star, as in the case of black holes. This is the first
self-consistent study where such a transition from sub-Keplerian flows has been
reported for neutron stars. We also identify the connection between accretion
and ejection of matter, following the Two-Component Advective Flow for black
holes, for neutron stars. The results are crucial in the understanding of the
formation of disks, boundary layers and outflows in wind dominated neutron star
systems.
