  The High Altitude Water Cherenkov (HAWC) telescope recently observed extended
emission around the Geminga and PSR~B0656+14 pulsar wind nebulae (PWNe). These
observations have been used to estimate cosmic-ray (CR) diffusion coefficients
near the PWNe that appear to be more than two orders of magnitude smaller than
that typically derived for the interstellar medium from the measured abundances
of secondary species in CRs. Two-zone diffusion models have been proposed as a
solution to this discrepancy, where the slower diffusion zone (SDZ) is confined
to a small region around the PWN. Such models are shown to successfully
reproduce the HAWC observations of the Geminga PWN while retaining consistency
with other CR data. It is found that the size of the SDZ influences the
predicted positron flux and the spectral shape of the extended $\gamma$-ray
emission at lower energies that can be observed with the {\it Fermi} Large Area
Telescope ({\it Fermi} LAT). If the two observed PWNe are not unique, then it
is likely that there are similar pockets of slow diffusion around many CR
sources elsewhere in the Milky Way. The consequences of such picture for
Galactic CR propagation is explored.
