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Kinetic Riemann simulations have been completed to explore particle heatingduring guide field reconnection in the low-$\beta$ environment of the innerheliosphere and the solar corona. The reconnection exhaust is bounded by tworotational discontinuities (RD) and two slow shocks (SS) form within theexhaust as in magnetohydrodynamic (MHD) models. At the RDs, ions areaccelerated by the magnetic field tension to drive the reconnection outflow aswell as flows in the out-of-plane direction. The out-of-plane flows streamtoward the midplane and meet to drive the SSs. The SSs differ greatly fromthose in the MHD model. The turbulence at the shock fronts and both upstreamand downstream is weak so the shocks are laminar and produce littledissipation. Downstream of the SSs the counterstreaming ion beams lead tohigher density, which leads to a positive potential between the SSs that actsto confine the downstream electrons to maintain charge neutrality. Thepotential accelerates electrons from upstream of the SSs to downstream regionand traps a small fraction but only modestly increases the downstream electrontemperature above the upstream value. In the low-$\beta$ limit the releasedmagnetic energy is split between bulk flow and ion heating with little energygoing to electrons. That the model does not produce strong electron heating noran energetic electron component suggests that other mechanisms, such asmultiple x-line reconnection, are required to explain energetic electronproduction in large flares. The model can be tested with the expected data fromthe Parker Solar Probe.

Particle Heating and Energy Partition in Low-$\beta$ Guide Field Reconnection with Kinetic Riemann Simulations