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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 theinteraction between the strong magnetic field of neutron star and the windmatter could cause such a long pulse period.  In this study, we follow the spin evolution of NS, taking into account theinteraction between the magnetic field and wind matter. In this line, as newchallenges, we solve the evolution of the magnetic field of the neutron star atthe same time, and additionally we focus on the effects of wind properties ofthe donor. As the result, evolutionary tracks were obtained in which theneutron star spends some duration in the ejector phase after birth, thenrapidly spins down, becomes quasi-equilibrium, and gradually spins up. Suchevolution is similar to previous studies, but we found that its dominantphysics depends on the velocity of the donor wind. When the wind velocity isfast, the spin-down occurs due to magnetic inhibition, while the classicalpropeller effect and settling accretion shell causes rapid spin-down in theslow wind accretion. Since the wind velocity of the donor could depend on theirradiated X-ray luminosity, the spin evolution track of the neutron star inwind-fed HMXB could be more complicated than considered.

Spin evolution of neutron stars in wind-fed high mass X-ray binaries