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High Mach number collisionless shocks are found in planetary systems andsupernova remnants (SNRs). Electrons are heated at these shocks to thetemperature well above the Rankine-Hugoniot prediction. However processesresponsible for electron heating are still not well understood. We use a set oflarge-scale Particle-In-Cell simulations of non-relativistic shocks in highMach number regime to clarify the electron heating processes. The physics ofthese shocks is defined by ion reflection at the shock ramp. Furtherinteraction of the reflected ions and the upstream plasma excites electrostaticBuneman and two-stream ion-ion Weibel instabilities. Electrons are heated viashock surfing acceleration, the shock potential, magnetic reconnection,stochastic Fermi scattering and the shock compression. The main contributor isthe shock potential. Magnetic field lines are tangled due to the Weibelinstability, which allows the parallel electron heating by the shock potential.The constrained model of the electron heating predicts the ion-to-electrontemperature ratio within observed values at SNR shocks and in Saturn's bowshock.

Kinetic simulation of nonrelativistic perpendicular shocks of young supernova remnants. IV. Electron heating