  Questions regarding energy dissipation in astrophysical jets are open to
date, despite of numerous attempts to limit the diversity of models. Some of
the most popular models assume that energy is transferred to particles via
internal shocks, which develop as a consequence of non-uniform velocity of the
jet matter. In this context, we study the structure and energy deposition of
colliding plasma shells, focusing our attention on the case of initially
inhomogeneous shells. This leads to formation of distorted (corrugated) shock
fronts -- a setup that has recently been shown to revive particle acceleration
in relativistic magnetized perpendicular shocks. Our studies show that the
radiative power of the far downstream of non-relativistic magnetized
perpendicular shocks is moderately enhanced with respect to the flat shock
cases. Based on the decay rate of downstream magnetic field, we make
predictions for multiwavelength polarization properties.
