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 gamma-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 gamma-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 $\gamma$-ray source should appear in addition to the presently observed the extended TeV gamma-ray source.