  The internal shocks scenario in relativistic jets is used to explain the
variability of the blazar emission. Recent studies have shown that the magnetic
field significantly alters the shell collision dynamics, producing a variety of
spectral energy distributions and light-curves patterns. However, the role
played by magnetization in such emission processes is still not entirely
understood. In this work we numerically solve the magnetohydodynamic evolution
of the magnetized shells collision, and determine the influence of the
magnetization on the observed radiation. Our procedure consists in
systematically varying the shell Lorentz factor, relative velocity, and viewing
angle. The calculations needed to produce the whole broadband spectral energy
distributions and light-curves are computationally expensive, and are achieved
using a high-performance parallel code.
