  Temporal changes of X-ray to very-high-energy gamma-ray emissions from the
pulsar-Be star binary PSR B1259-63/LS 2883 are studied based on 3-D SPH
simulations of pulsar wind interaction with Be-disk and wind. We focus on the
periastron passage of the binary and calculate the variation of the synchrotron
and inverse-Compton emissions using the simulated shock geometry and pressure
distribution of the pulsar wind. The characteristic double-peaked X-ray light
curve from observations is reproduced by our simulation under a dense Be disk
condition (base density ~10^{-9} g cm^{-3}). We interpret the pre- and
post-periastron peaks as being due to a significant increase in the conversion
efficiency from pulsar spin down power to the shock-accelerated particle energy
at orbital phases when the pulsar crosses the disk before periastron passage,
and when the pulsar wind creates a cavity in the disk gas after periastron
passage, respectively. On the contrary, in the model TeV light curve, which
also shows a double peak feature, the first peak appears around the periastron
phase. The possible effects of cooling processes on the TeV light curve are
briefly discussed.
