High Energy Emission from the Double Pulsar system J0737-3039

Abstract

We discuss the effects of particle acceleration at the bow shocks expected in the binary pulsar system J0737-3039, due to the wind from pulsar A interacting with both the interstellar medium (ISM), and with 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 $\lesssim$ 60 keV, at a level of $\sim 2 \times 10^{-13}$ erg cm$^{-2}$ s$^{-1}$.

accepted to ApJL; clearer presentation and improved estimate for the high energy emission