Gamma-rays from comptonization of stellar radiation in the binary system containing PSR J2032+4127 at its periastron passage

Abstract

We calculate the high energy gamma-ray emission expected during the periastron passage of the pulsar PSR J2032+4127 which form extended binary system with the massive companion star MT91 213. The γ-ray emission is expected due to the comptonization of the stellar radiation by electrons accelerated at the pulsar wind and stellar wind collision shock. We apply the numerical code for the cascade process initiated by electrons in the anisotropic radiation from the companion star. We conclude that around the periastron passage of this binary system, the γ-ray emission at TeV energies can overcome the TeV emission observed from an extended source in this direction which is likely due to the pulsar wind nebula formed by the pulsar PSR J2032+4127. We discuss the conditions within the binary system for which such a point like TeV γ-ray source should appear in addition to the presently observed the extended TeV γ-ray source.

Status of ground based gamma-ray observations

“…The periastron of this system will be around November of 2017, providing a unique opportunity to study the system [29]. It is expected for VHE gammaray emission to reach to the highest flux level between periastron and superior conjunction [30]. Depending on the efficiency of the acceleration and the environmental conditions, the gamma-ray emission may overcome the emission from TeV J2032+4130.…”