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PSR J2032+4127 is a radio-loud gamma-ray-emitting pulsar; it is orbitingaround a high-mass Be type star with a very long orbital period of 25-50years,and is approaching periastron, which will occur in late 2017/early 2018. Thissystem comprises with a young pulsar and a Be type star, which is similar tothe so-called gamma-ray binary PSR~B1259-63/LS2883. It is expected thereforethat PSR J2032+4127 shows an enhancement of high-energy emission caused by theinteraction between the pulsar wind and Be wind/disk around periastron. Ho etal. recently reported a rapid increase in the X-ray flux from this system. Inthis paper, we also confirm a rapid increase in the X-ray flux along the orbit,while the GeV flux shows no significant change. We discuss the high-energyemissions from the shock caused by the pulsar wind and stellar wind interactionand examine the properties of the pulsar wind in this binary system. We arguethat the rate of increase of the X-ray flux observed by Swift indicates (1) avariation of the momentum ratio of the two-wind interaction region along theorbit, or (2) an evolution of the magnetization parameter of the pulsar windwith the radial distance from the pulsar. We also discuss the pulsar wind/Bedisk interaction at the periastron passage, and propose the possibility offormation of an accretion disk around the pulsar. We model high-energyemissions through the inverse-Compton scattering process of thecold-relativistic pulsar wind off soft photons from the accretion disk.

High-Energy emissions from the Pulsar/Be binary system PSR J2032+4127/MT91 213