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We can probe observationally and reproduce theoretically intricate propertiesof the Crab Nebula nearest to the pulsar - The Inner Knot. The tiny knot isindeed a bright spot on the surface of a quasi-stationary magnetic relativisticshock that accelerates particles. It is required that the part of the wind thatproduces the Inner Knot has low magnetization; thus, it is not a site ofgamma-ray flares.  We develop a model of particle acceleration during explosive reconnectionevents in relativistic highly magnetized plasma and apply the model to explainthe Crab gamma-ray flares. Particles are efficiently accelerated bycharge-starved DC-type electric fields during initial stages of magnetic fluxmerges. By implication, the magnetic reconnection is an important, and possiblydominant process of particle acceleration in high energy astrophysical sources.

What we recently learnt about Crab: structure of the wind, the shock, flares and reconnection