High-energy emission from the double pulsar system J0737-3039

We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, because of the wind from pulsar A interacting with both the interstellar medium (ISM) and the magnetosphere of pulsar B. In this model, we find that the likeliest source for the X-rays observed by Chandra is the emission from the shocked wind of pulsar A as it interacts with the ISM. In this case, for favorable model parameter values, better statistics might help Chandra marginally resolve the source. A consequence of the model is a power-law high-energy spectrum extending up to ≲60 keV, at a level of ∼2 × 10^-13 ergs cm ^-2s^-1.