  HESS J0632+057 is an eccentric gamma-ray Be binary that produces non-thermal
radio, X-rays, GeV, and very high-energy gamma rays. The non-thermal emission
of HESS J0632+057 is modulated with the orbital period, with a dominant maximum
before apastron passage. The nature of the compact object in HESS J0632+057 is
not known, although it has been proposed to be a young pulsar as in PSR
B1259-63, the only gamma-ray emitting high-mass binary known to host a
non-accreting pulsar. In this Letter, we present hydrodynamical simulations of
HESS J0632+057 in the context of a pulsar and a stellar wind interacting in an
eccentric binary, and propose a scenario for the non-thermal phenomenology of
the source. In this scenario, the non-thermal activity before and around
apastron is linked to the accumulation of non-thermal particles in the vicinity
of the binary, and the sudden drop of the emission before apastron is produced
by the disruption of the two-wind interaction structure, allowing these
particles to efficiently escape. In addition to providing a framework to
explain the non-thermal phenomenology of the source, this scenario predicts
extended, moving X-ray emitting structures similar to those observed in PSR
B1259-63.
