  The binary system HESS J0632+057 was recently detected by {Fermi} to possess
orbital modulated GeV emission. In this paper, we study the possibility that
the compact companion of HESS J0632+057 is a pulsar. Under such a presumption,
we focus on the high energy emission mechanism of this system, which is as
follows. The pulsar companion travels through the circumstellar disc of the
main sequence star twice in each orbit, when some of the matter is
gravity-captured. The captured matter develops an accretion disc around the
pulsar, and the soft photons from which are inverse Compton scattered by the
pulsar wind as the GeV emission from the system. With proper choice of
parameters, SED and light curve which are in accordance with observations can
be produced. We predict that the light curve of GeV emission has two peaks, the
larger one is at around 0.4 after the periastron (or 0.1 after the X-ray
maximum), while the smaller one is between phases 0 and 0.1, with integrated
flux one forth of the larger one.
