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The recent detection of gravitational waves associated with a binary neutronstar merger revives interest in interacting pulsar magnetospheres. Currentmodels predict that a significant amount of magnetic energy should be releasedprior to the merger, leading to electromagnetic precursor emission. In thispaper, we revisit this problem in the light of the recent progress in kineticmodeling of pulsar magnetospheres. We limit our work to the case of alignedmagnetic moments and rotation axes, and thus neglect the orbital motion. Weperform global two-dimensional axisymmetric particle-in-cell simulations of twopulsar magnetospheres merging at a rate consistent with the emission ofgravitational waves. Both symmetric and asymmetric systems are investigated.Simulations show a significant enhancement of magnetic dissipation within themagnetospheres as both stars get closer. Even though the magnetosphericconfiguration depends on the relative orientations of the pulsar spins andmagnetic axes, all configurations present nearly the same radiative signature,indicating that a common dissipation mechanism is at work. The relative motionof both pulsars drives magnetic reconnection at the boundary between the twomagnetospheres, leading to efficient particle acceleration and high-energysynchrotron emission. Polar-cap discharge is also strongly enhanced inasymmetric configurations, resulting in vigorous pair production andpotentially additional high-energy radiation. We observe an increase in thepulsar radiative efficiency by two orders of magnitude over the last orbitbefore the merger exceeding the spindown power of an isolated pulsar. Theexpected signal is too weak to be detected at high energies even in the nearbyuniverse. However, if a small fraction of this energy is channeled into radiowaves, it could be observed as a non-repeating fast radio burst.

Kinetic modeling of the electromagnetic precursor from an axisymmetric binary pulsar coalescence