  Using the formulation of relativistic reconnection by Lyutikov & Uzdensky
(2002) we estimate the upper possible rates of reconnection in pulsar winds
using Bohm prescription for resistivity. We find that the velocity of plasma
inflow into the reconnection layer may be relativistic, of the order of the
speed of light in the plasma rest-frame. This in principle may allow efficient
dissipation of the magnetic field energy in the wind and/or destruction of the
toroidal magnetic flux.
  The efficiency of reconnection realized in pulsar winds remains an open
question: it should depend both on the microphysical properties of plasma and
on the three-dimensional structure of the reconnection flow.
