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We propose that magnetic reconnection at the heliopause only occurs where theinterstellar magnetic field points nearly anti-parallel to the heliosphericfield. By using large-scale magnetohydrodynamic (MHD) simulations of theheliosphere to provide the initial conditions for kinetic simulations ofheliopause (HP) reconnection we show that the energetic pickup ions downstreamfrom the solar wind termination shock induce large diamagnetic drifts in thereconnecting plasma and stabilize non-anti-parallel reconnection. With thisconstraint the MHD simulations can show where HP reconnection most likelyoccurs. We also suggest that reconnection triggers the 2-3 kHz radio burststhat emanate from near the HP. Requiring the burst locations to coincide withthe loci of anti-parallel reconnection allows us to determine, for the firsttime, the vector direction of the local interstellar magnetic field. We find itto be oriented towards the southern solar magnetic pole.

The Vector Direction of the Interstellar Magnetic Field Outside the Heliosphere