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Supernovae (SNe) with strong interactions with circumstellar material (CSM)are promising candidate sources of high-energy neutrinos and gamma rays, andhave been suggested as an important contributor to Galactic cosmic rays beyond1 PeV. Taking into account the shock dissipation by a fast velocity componentof SN ejecta, we present comprehensive calculations of the non-thermal emissionfrom SNe powered by shock interactions with a dense wind or CSM. Remarkably, weconsider electromagnetic cascades in the radiation zone and subsequentattenuation in the pre-shock CSM. A new time-dependent phenomenologicalprescription provided by this work enables us to calculate gamma-ray, hardX-ray, radio, and neutrino signals, which originate from cosmic raysaccelerated by the diffusive shock acceleration mechanism. We apply our resultsto SN IIn 2010jl and SN Ib/IIn 2014C, for which the model parameters can bedetermined from the multi-wavelength data. For SN 2010jl, the more promisingcase, by using the the latest Fermi Large Area Telescope (LAT) Pass 8 datarelease, we derive new constraints on the cosmic-ray energy fraction,<0.05-0.1. We also find that the late-time radio data of these interacting SNeare consistent with our model. Further multi-messenger and multi-wavelengthobservations of nearby interacting SNe should give us new insights into thediffusive shock acceleration in dense environments as well as pre-SN mass-lossmechanisms.

High-Energy Emission from Interacting Supernovae: New Constraints on Cosmic-Ray Acceleration in Dense Circumstellar Environments