  In this paper, we model the dynamics and radiation physics of the rarity
event GRB 221009A afterglow in detail. By introducing a top-hat jet that
propagates in an environment dominated by stellar winds, we explain the
publicly available observations of afterglow associated with GRB 221009A over
the first week. It is predicted that GRB 221009A emits a luminous very high
energy (VHE) afterglow based on the synchrotron self-Compton (SSC) process in
our model. We show the broadband spectral energy distribution (SED) analysis
results of GRB 221009A, and find that the SSC radiation component of GRB
221009A is very bright in the 0.1 - 10 TeV band. The integrated SED shows that
the SSC emission in the TeV band has significantly higher than the detection
sensitivity of LHASSO, MAGIC and CTA. However, since the release of further
observations, deviations from the standard wind environment model gradually
show up in data. For example, the late-time multiband afterglow cannot be
consistently explained under the standard wind environment scenario. It may be
necessary to consider modeling with a structured jet with complex geometry or a
partial revision of the standard model. Furthermore, we find that the inclusion
of GeV observations could break the degeneracy between model parameters,
highlighting the significance of high-energy observations in determining
accurate parameters for GRB afterglows.
