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

## TL;DR

This study investigates high-energy emissions from the PSR J2032+4127/MT91 213 binary system, analyzing X-ray flux variations and modeling emission processes to understand pulsar wind interactions near periastron.

## Contribution

It provides new insights into the high-energy emission mechanisms and pulsar wind properties in a long-period Be star binary system during periastron.

## Key findings

- Rapid increase in X-ray flux observed along the orbit.
- GeV flux remains relatively unchanged.
- Model suggests inverse-Compton scattering of pulsar wind off disk photons.

## Abstract

PSR J2032+4127 is a radio-loud gamma-ray-emitting pulsar; it is orbiting around 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. This system comprises with a young pulsar and a Be type star, which is similar to the so-called gamma-ray binary PSR~B1259-63/LS2883. It is expected therefore that PSR J2032+4127 shows an enhancement of high-energy emission caused by the interaction between the pulsar wind and Be wind/disk around periastron. Ho et al. recently reported a rapid increase in the X-ray flux from this system. In this 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-energy emissions from the shock caused by the pulsar wind and stellar wind interaction and examine the properties of the pulsar wind in this binary system. We argue that the rate of increase of the X-ray flux observed by Swift indicates (1) a variation of the momentum ratio of the two-wind interaction region along the orbit, or (2) an evolution of the magnetization parameter of the pulsar wind with the radial distance from the pulsar. We also discuss the pulsar wind/Be disk interaction at the periastron passage, and propose the possibility of formation of an accretion disk around the pulsar. We model high-energy emissions through the inverse-Compton scattering process of the cold-relativistic pulsar wind off soft photons from the accretion disk.