  PSR B1259-63/SS 2883 is a binary system in which a 48-ms pulsar orbits around
a Be star in a high eccentric orbit with a long orbital period of about 3.4 yr.
Extensive broadband observational data are available for this system from radio
band to very high energy (VHE) range. The multi-frequency emission is unpulsed
and nonthermal, and is generally thought to be related to the relativistic
electrons accelerated from the interaction between the pulsar wind and the
stellar wind, where X-ray emission is from the synchrotron process and the VHE
emission is from the inverse Compton (IC) scattering process. Here a shocked
wind model with variation of the magnetic parameter $\sigma$ is developed for
explaining the observations. By choosing proper param- eters, our model could
reproduce two-peak profile in X-ray and TeV light curves. The effect of the
disk exhibits an emission and an absorption components in the X-ray and TeV
bands respectively. We suggest that some GeV flares will be produced by Doppler
boosting the synchrotron spectrum. This model can possibly be used and be
checked in other similar systems such as LS I+61o303 and LS 5039.
