  We investigated a wealth of X-ray and gamma-ray spectral energy distribution
(SED) and multi-band light curve (LC) data of the gamma-ray binary HESS
J0632+057 using a phenomenological intrabinary shock (IBS) model. Our baseline
model assumes that the IBS is formed by colliding winds from a putative pulsar
and its Be companion, and particles accelerated in the IBS emit broadband
radiation via synchrotron (SY) and inverse-Compton upscattering (ICS)
processes. Adopting the latest orbital solution and system geometry (Tokayer et
al. 2021), we reproduced the global X-ray and TeV LC features, two broad bumps
at $\phi \sim 0.3$ and $\sim0.7$, with the SY and ICS model components. We
found these TeV LC peaks originate from ICS emission caused by the enhanced
seed photon density near periastron and superior conjunction or Doppler-beamed
emission of bulk-accelerated particles in the IBS at inferior conjunction.
While our IBS model successfully explained most of the observed SED and LC
data, we found that phase-resolved SED data in the TeV band require an
additional component associated with ICS emission from pre-shock particles
(produced by the pulsar wind). This finding indicates a possibility of
delineating the IBS emission components and determining the bulk Lorentz
factors of the pulsar wind at certain orbital phases.
