  We construct a turbulent model of the Crab Nebula's non-thermal emission. The
present model resolves a number of long-standing problems of the
Kennel-Coroniti (1984) model: (i) the sigma problem; (ii) the hard spectrum of
radio electrons; (iii) the high peak energy of gamma-ray flares; (iv) and the
spacial evolution of the infrared (IR) emission. The Nebula contains two
populations of injected particles: Component-I accelerated at the wind
termination shock via Fermi-I mechanism, and Component-II accelerated in
reconnecting turbulence in highly magnetized ($\sigma$ $\gg 1$) plasma in the
central part of the Crab Nebula. The reconnecting turbulence Component-II
extends from radio to gamma rays: it accelerate radio electrons with a hard
spectrum, destroy the large scale magnetic flux (and thus resolves the
sigma-problem), and occasionally produces gamma-ray flares (from the largest
scale reconnection events). The model reproduces the broad-band spectrum of the
Crab Nebula, from low-frequency synchrotron emission in radio to
inverse-Compton emission at TeV energies, as well as spatially resolved
evolution of the spectral indices in IR and optical bands.
