Speaker
Description
The gamma-ray binary is composed of the compact object (pulsar/black hole)
and high mass OB star, and is gamma-ray loud object. In this talk, I will focus on recent theoretical and observational studies for the gamma-ray binary hosting Be star.
For PSR B1259-63/LS 2883, the origin of flare-like GeV emission after the second disk passage is puzzling, and it may be interpreted as a consequence of the inverse-Compton process of the pulsar wind scattering off the soft photon from
the accretion disk around the pulsar. For HESSJ0632+057,
the recent optical/X-ray studies indicate a shorter
orbital period and a smaller eccentricity than those reported
in previous. Phase positions of the observed X-ray flare and dip
are modified by new orbital parameters. PSR J2032+4127/MT91 213 is the candidate of the gamma-ray binary with a orbit period ~50 years. The X-ray flux from this system rapidly increases with flare-like activities, as the pulsar approaches to the periastron in late 2017/early 2018.
I will also report new feature of the super orbital modulation of LS I +61$^{\circ}$303 using ~8 years Fermi-LAT data.
