  The observed X-ray pulse period of OB-type high-mass X-ray binary (HMXB)
pulsars are typically longer than 100 seconds. It is considered that the
interaction between the strong magnetic field of neutron star and the wind
matter could cause such a long pulse period.
  In this study, we follow the spin evolution of NS, taking into account the
interaction between the magnetic field and wind matter. In this line, as new
challenges, we solve the evolution of the magnetic field of the neutron star at
the same time, and additionally we focus on the effects of wind properties of
the donor. As the result, evolutionary tracks were obtained in which the
neutron star spends some duration in the ejector phase after birth, then
rapidly spins down, becomes quasi-equilibrium, and gradually spins up. Such
evolution is similar to previous studies, but we found that its dominant
physics depends on the velocity of the donor wind. When the wind velocity is
fast, the spin-down occurs due to magnetic inhibition, while the classical
propeller effect and settling accretion shell causes rapid spin-down in the
slow wind accretion. Since the wind velocity of the donor could depend on the
irradiated X-ray luminosity, the spin evolution track of the neutron star in
wind-fed HMXB could be more complicated than considered.
