  We have studied several neutron star high-mass X-ray binaries (HMXBs) with
super-giant (SG) companions using a wind-fed binary model associated with the
magnetic field. By using the concept of torque balance, the magnetic field
parameter determines the mass accretion rate. This would help us to consider
the relationship between wind velocity and mass-loss rate. These parameters
significantly improve our understanding of the accretion mechanism. The wind
velocity is critical in determining the X-ray features. This can be used to
identify the ejection process and the stochastic variations in their accretion
regimes. However, even in systems with a long orbital period, an accretion disk
can be created when the wind velocity is slow. This will allow the HMXB of both
types, SG and Be, to be better characterised by deriving accurate properties
from these binaries. In addition, we have performed segmentation in the
parameter space of donors intended for several SG-HMXB listed in our sample
set. The parameter space can be categorised into five regimes, depending on the
possibility of disk formation associated with accretion from the stellar wind.
This can give a quantitative clarification of the observed variability and the
properties of these objects. For most of the systems, we show that the derived
system parameters are consistent with the assumption that the system is
emitting X-rays through direct accretion. However, there are some sources (LMC
X-4, Cen X-3 and OAO1657-415) that are not in the direct accretion regime,
although they share similar donor parameters. This may indicate that these
systems are transitioning from a normal wind accretion phase to partial RLOF
regimes.
