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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 HESSJ0632+057 using a phenomenological intrabinary shock (IBS) model. Our baselinemodel assumes that the IBS is formed by colliding winds from a putative pulsarand its Be companion, and particles accelerated in the IBS emit broadbandradiation via synchrotron (SY) and inverse-Compton upscattering (ICS)processes. Adopting the latest orbital solution and system geometry (Tokayer etal. 2021), we reproduced the global X-ray and TeV LC features, two broad bumpsat $\phi \sim 0.3$ and $\sim0.7$, with the SY and ICS model components. Wefound these TeV LC peaks originate from ICS emission caused by the enhancedseed photon density near periastron and superior conjunction or Doppler-beamedemission of bulk-accelerated particles in the IBS at inferior conjunction.While our IBS model successfully explained most of the observed SED and LCdata, we found that phase-resolved SED data in the TeV band require anadditional component associated with ICS emission from pre-shock particles(produced by the pulsar wind). This finding indicates a possibility ofdelineating the IBS emission components and determining the bulk Lorentzfactors of the pulsar wind at certain orbital phases.

Investigation of the broadband emission of the gamma-ray binary HESS J0632+057 using an intrabinary shock model