  Recent results from LHAASO and Tibet AS$\gamma$ suggest that the Crab
Nebula's gamma-ray spectrum extends to the PeV energy range, however the
production mechanisms of this highest energy emission remain unclear. It has
been postulated that a secondary component of hadronic emission could explain
the highest energy gamma-ray flux points, however the origin and acceleration
mechanism for this hadronic population has yet to be explained. We postulate
one scenario in which hadrons diffuse over time into the Crab pulsar wind
nebula from the surrounding supernova ejecta, and are subsequently
re-accelerated by the pulsar wind termination shock. We present results of
direct particle transport simulations (including radial evolution) to determine
if this scenario is viable over the lifetime of the Crab system.
