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Synchrotron radiation from relativistic electrons is usually invoked as theresponsible for the nonthermal emission observed in Supernova Remnants (SNRs).Diffusive shock acceleration (DSA) is the most popular mechanism to explain theprocess of particles acceleration and within its framework a crucial role isplayed by the turbulent magnetic-field. However, the standard models commonlyused to fit X-ray synchrotron emission do not take into account the effects ofturbulence in the shape of the resulting photon spectra. An alternativemechanism that properly includes such effects is the jitter radiation, thatprovides for an additional power-law beyond the classical synchrotron cutoff.We fitted a jitter spectral model to Chandra, NuSTAR, SWIFT/BAT andINTEGRAL/ISGRI spectra of Cassiopeia A and found that it describes the X-raysoft-to-hard range better than any of the standard cutoff models. The jitterradiation allows us to measure the index of the magnetic turbulence spectrum$\nu_B$ and the minimum scale of the turbulence $\lambda_{\rm{min}}$ acrossseveral regions of Cas A, with best-fit values $\nu_B \sim 2-2.4$ and$\lambda_{\rm{min}} \lesssim 100$ km.

Jitter radiation as an alternative mechanism for the nonthermal X-ray emission of Cassiopeia A