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Synchrotron X-ray emission in young supernova remnants (SNRs) is a powerfuldiagnostic tool to study the population of high energy electrons accelerated atthe shock front and the acceleration process. We performed a spatially resolvedspectral analysis of NuSTAR and XMM-Newton observations of the young Kepler'sSNR, aiming to study in detail its non-thermal emission in hard X-rays. Weselected a set of regions all around the rim of the shell and extracted thecorresponding spectra. The spectra were analyzed by adopting a model ofsynchrotron radiation in the loss-limited regime, to constrain the dependenceof the cutoff energy of the synchrotron radiation on the shock velocity. Weidentify two different regimes of particle acceleration, characterized bydifferent Bohm factors. In the north, where the shock interacts with a densecircumstellar medium (CSM), we found a more efficient acceleration than in thesouth, where the shock velocity is higher and there are no signs of shockinteraction with dense CSM. Our results suggest an enhanced efficiency of theacceleration process in regions where the shock-CSM interaction generates anamplified and turbulent magnetic field. By combining hard X-ray spectra withradio and $\gamma-$ray observations of Kepler's SNR, we modelled the spectralenergy distribution. In the light of our results we propose that the observed$\gamma-$ray emission is mainly hadronic, and originates in the northern partof the shell.

A spatially resolved study of hard X-ray emission in Kepler's SNR: indications of different regimes of particle acceleration