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The supernova remnant SN 1006 is a source of high-energy particles and itssouthwestern limb is interacting with a dense ambient cloud, thus being apromising region for gamma-ray hadronic emission. We aim at describing thephysics and the nonthermal emission associated with the shock-cloud interactionto derive the physical parameters of the cloud (poorly constrained by the dataanalysis), to ascertain the origin of the observed spatial variations in thespectral properties of the X-ray synchrotron emission, and to predict spectraland morphological features of the resulting gamma-ray emission. We performed3-D magnetohydrodynamic simulations modeling the evolution of SN 1006 and itsinteraction with the ambient cloud, and explored different model setups. Byapplying the REMLIGHT code on the model results, we synthesized the synchrotronX-ray emission, and compared it with actual observations, to constrain theparameters of the model. We also synthesized the leptonic and hadronicgamma-ray emission from the models, deriving constraints on the energy contentof the hadrons accelerated at the southwestern limb. We found that the impactof the SN 1006 shock front with a uniform cloud with density 0.5 cm^-3 canexplain the observed morphology, the azimuthal variations of the cutofffrequency of the X-ray synchrotron emission, and the shock proper motion in theinteraction region. Our results show that the current upper limit for the totalhadronic energy in the southwestern limb is 2.5e49 erg.

Modeling the shock-cloud interaction in SN 1006: unveiling the origin of nonthermal X-ray and gamma-ray emission