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Supernova remnants are known to accelerate cosmic-rays from the detection ofnon-thermal emission in radio waves, X-rays, and gamma-rays. However, theability to accelerate cosmic-rays up to PeV energies has yet to bedemonstrated. The presence of cut-offs in the gamma-ray spectra of severalyoung SNRs led to the idea that PeV energies might only be achieved during thefirst years of a remnant's evolution. We use our time-dependentacceleration-code RATPaC to study the acceleration of cosmic-rays in supernovaeexpanding into dense environments around massive stars. We performedspherically symmetric 1-D simulations in which we simultaneously solve thetransport equations for cosmic-rays, magnetic turbulence, and thehydrodynamical flow of the thermal plasma in the test-particle limit. Weinvestigated typical CSM parameters expected around RSG and LBV stars forfreely expanding winds and accounted for the strong gamma-gamma-absorption inthe first days after explosion. The maximum achievable particle energy islimited to below 600TeV even for largest considered values of the magneticfield and mass-loss rates. The maximum energy is not expected to surpass 200TeVand 70TeV for LBVs and RSGs that experience moderate mass-loss prior to theexplosion. We find gamma-ray peak-luminosities consistent with current upperlimits and evaluated that current-generation instruments are able to detect thegamma-rays from Type-IIP explosions at distances up to 60kpc and Type-IInexplosions up to 1.0Mpc. We also find a good agreement between the thermalX-ray and radio synchrotron emission predicted by our models with a range ofobservations.

Core-collapse supernovae in dense environments -- particle acceleration and non-thermal emission