  PSR J2032+4127 is a young and rapidly rotating pulsar on a highly eccentric
orbit around the high-mass Be star MT91 213. X-ray monitoring of the binary
system over a $\sim$4000 day period with Swift has revealed an increase of the
X-ray luminosity which we attribute to the synchrotron emission of the shocked
pulsar wind. We use Swift X-ray observations to infer a clumpy stellar wind
with $r^{-2}$ density profile and constrain the Lorentz factor of the pulsar
wind to $10^5<\gamma_w<10^6$. We investigate the effects of an axisymmetric
stellar wind with polar gradient on the X-ray emission. Comparison of the X-ray
light curve hundreds of days before and after the periastron can be used to
explore the polar structure of the wind.
