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In situ observations of energetic particles at the Earth's bow-shock that areattainable by the satellite missions have long created the opinion thatelectrons are most efficiently accelerated in a quasi-perpendicular shockgeometry. However, shocks that are deemed to be responsible for the productionof cosmic ray electrons and their radiation from sources such as supernovaremnants are much more powerful and larger than the Earth's bow-shock. Theirremote observations and in situ measurements at Saturn's bow shock, suggestthat electrons are accelerated very efficiently in the quasi-parallel shocks aswell. In this paper we investigate the possibility that protons that areaccelerated to high energies create sufficient wave turbulence, which isnecessary for the electron preheating and subsequent injection into thediffusive shock acceleration in a quasi-parallel shock geometry. An additionaltest-particle-electron population, which is meant to be a low-density additionto the electron core-distribution on which the hybrid simulation operates, isintroduced. We investigate how these electrons are energized by the hybridelectromagnetic field. The reduced spatial dimensionality allowed us todramatically increase the number of macro-ions per numerical cell and achievethe converged results for the velocity distributions of test electrons. Wediscuss the electron preheating mechanisms, which can make a significant partof thermal electrons accessible to the ion-driven waves observed in hybridsimulations. We find that the precursor wave field supplied by ions has aconsiderable potential to preheat the electrons before they are shocked at thesubshock.

Electron Energization in Quasi-Parallel Shocks: Test-Particle-Electrons in a Proton Driven Turbulence