Perpendicular relativistic ( \gamma _ { 0 } = 10 ) shocks in magnetized pair plasmas are investigated using two dimensional Particle-in-Cell simulations .
A systematic survey , from unmagnetized to strongly magnetized shocks , is presented accurately capturing the transition from Weibel-mediated to magnetic-reflection-shaped shocks .
This transition is found to occur for upstream flow magnetizations 10 ^ { -3 } < \sigma < 10 ^ { -2 } at which a strong perpendicular net current is observed in the precursor , driving the so-called current-filamentation instability .
The global structure of the shock and shock formation time are discussed .
The MHD shock jump conditions are found in good agreement with the numerical results , except for 10 ^ { -4 } < \sigma < 10 ^ { -2 } where a deviation up to 10 % is observed .
The particle precursor length converges toward the Larmor radius of particles injected in the upstream magnetic field at intermediate magnetizations .
For \sigma > 10 ^ { -2 } , it leaves place to a purely electromagnetic precursor following from the strong emission of electromagnetic waves at the shock front .
Particle acceleration is found to be efficient in weakly magnetized perpendicular shocks in agreement with previous works , and is fully suppressed for \sigma > 10 ^ { -2 } .
Diffusive Shock Acceleration is observed only in weakly magnetized shocks , while a dominant contribution of Shock Drift Acceleration is evidenced at intermediate magnetizations .
The spatial diffusion coefficients are extracted from the simulations allowing for a deeper insight into the self-consistent particle kinematics and scale with the square of the particle energy in weakly magnetized shocks .
These results have implications for particle acceleration in the internal shocks of AGN jets and in the termination shocks of Pulsar Wind Nebulae .