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PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbitingaround a O9.5Ve star, LS 2883, with a period of ~3.4 years. The interaction ofthe pulsar wind with the LS 2883 outflow leads to unpulsed broad band emissionin the radio, X-rays, GeV and TeV domains. While the radio, X-ray and TeV lightcurves show rather similar behaviour, the GeV light curve appears verydifferent with a huge outburst about a month after a periastron. The energyrelease during this outburst seems to significantly exceed the spin downluminosity of the pulsar and the GeV light curve and energy release varies fromone orbit to the next.  In this paper we present for the first time the results of opticalobservations of the system in 2017, and also reanalyze the available X-ray andGeV data. We present a new model in which the GeV data are explained as acombination of the bremsstrahlung and inverse Compton emission from theunshocked and weakly shocked electrons of the pulsar wind. The X-ray and TeVemission is produced by synchrotron and inverse Compton emission of energeticelectrons accelerated on a strong shock arising due to stellar/pulsar windscollision. The brightness of the GeV flare is explained in our model as abeaming effect of the energy released in a cone oriented, during the time offlare, in the direction of the observer.

New insight into the origin of the GeV flare in the binary system PSR B1259-63 from the 2017 periastron passage