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Weakly magnetized, relativistic collisionless shock waves are not only thenatural offsprings of relativistic jets in high-energy astrophysical sources,they are also associated with some of the most outstanding displays of energydissipation through particle acceleration and radiation. Perhaps their mostpeculiar and exciting feature is that the magnetized turbulence that sustainsthe acceleration process, and (possibly) the secondary radiation itself, isself-excited by the accelerated particles themselves, so that the phenomenologyof these shock waves hinges strongly on the microphysics of the shock. In thisreview, we draw a status report of this microphysics, benchmarking analyticalarguments with particle-in-cell simulations, and extract consequences of directinterest to the phenomenology, regarding in particular the so-calledmicrophysical parameters used in phenomenological studies.

Physics and phenomenology of weakly magnetized, relativistic astrophysical shock waves