We outline a model of the Crab Pulsar Wind Nebula with two different populations of synchrotron emitting particles , arising from two different acceleration mechanisms : ( i ) Component-I due to Fermi-I acceleration at the equatorial portion of the termination shock , with particle spectral index p _ { I } \approx 2.2 above the injection break corresponding to \gamma _ { wind } \sigma _ { wind } \sim 10 ^ { 5 } , peaking in the UV ( \gamma _ { wind } \sim 10 ^ { 2 } is the bulk Lorentz factor of the wind , \sigma _ { wind } \sim 10 ^ { 3 } is wind magnetization ) ; ( ii ) Component-II due to acceleration at reconnection layers in the bulk of the turbulent Nebula , with particle index p _ { II } \approx 1.6 .
The model requires relatively slow but highly magnetized wind .
For both components the overall cooling break is in the infra-red at \sim 0.01 eV , so that the Component-I is in the fast cooling regime ( cooling frequency below the peak frequency ) .
In the optical band Component-I produces emission with the cooling spectral index of \alpha _ { o } \approx 0.5 , softening towards the edges due to radiative losses .
Above the cooling break , in the optical , UV and X-rays , Component-I mostly overwhelms Component-II .
We hypothesize that acceleration at large-scale current sheets in the turbulent nebula ( Component-II ) extends to the synchrotron burn-off limit of \epsilon _ { s } \sim 100 MeV .
Thus in our model acceleration in turbulent reconnection ( Component-II ) can produce both hard radio spectra and occasional gamma-ray flares .
This model may be applicable to a broader class of high energy astrophysical objects , like AGNe and GRB jets , where often radio electrons form a different population from the high energy electrons .