  Nearby pulsars have been suggested as sources of $\sim$TeV $e^+/e^-$ Cosmic
Ray (CR) excess on Earth. The High-Altitude Water Cherenkov Observatory (HAWC)
detected extended TeV emission regions in the direction of two nearby
middle-aged pulsars, Geminga and PSR B0656+14. By modeling the TeV emission as
inverse Compton emission from electron-positron pairs diffusing in the
interstellar medium (ISM), the HAWC collaboration derives a diffusion
coefficient much smaller than the standard value in the vicinity of the two
pulsars, which make them unlikely the origin of the positron excess. We propose
that the observed $\gamma$-ray emission originate from the relic pulsar wind
nebula. A two zone diffusion model with a slow diffusion in the nebula and a
fast diffusion in the ISM can explain the HAWC surface brightness profile and
the positron excess simultaneously. Inefficient diffusion in the $\gamma$-ray
emission region surrounding a middle-aged pulsar maybe a common phenomenon that
can be tested by future observation. The implied diffusion coefficient in the
ISM is smaller than the one suggested by the standard CR propagation model, but
it is fully consistent with the predictions of the spiral arm model.
