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The internal shocks scenario in relativistic jets is used to explain thevariability of the blazar emission. Recent studies have shown that the magneticfield significantly alters the shell collision dynamics, producing a variety ofspectral energy distributions and light-curves patterns. However, the roleplayed by magnetization in such emission processes is still not entirelyunderstood. In this work we numerically solve the magnetohydodynamic evolutionof the magnetized shells collision, and determine the influence of themagnetization on the observed radiation. Our procedure consists insystematically varying the shell Lorentz factor, relative velocity, and viewingangle. The calculations needed to produce the whole broadband spectral energydistributions and light-curves are computationally expensive, and are achievedusing a high-performance parallel code.

Numerical simulations of the internal shock model in magnetized relativistic jets of blazars