  We analyse the damping by radiation reaction and by Compton drag of strong,
superluminal electromagnetic waves in the context of pulsar winds. The
associated radiation signature is found by estimating the efficiency and the
characteristic radiation frequencies. Applying these estimates to the gamma-ray
binary containing PSR B1259-63, we show that the GeV flare observed by
Fermi-LAT can be understood as inverse Compton emission by particles scattering
photons from the companion star, if the pulsar wind termination shock acquires
a precursor of superluminal waves roughly 30 days after periastron. This
constrains the mass-loading factor of the wind $\mu=L/\dot{N}mc^2$ (where $L$
is the luminosity and $\dot{N}$ the rate of loss of electrons and positrons) to
be roughly $6\times 10^4$.
