The complex environments around core-collapse supernova remnants (SNRs) originates from their massive progenitors and shapes the spectra and morphology of non-thermal emissions from the remnants.
We study the effects of the flow profiles and the magnetic field of the circumstellar medium on particle acceleration and emission from remnants and estimate the contribution of core-collapse SNRs to the Galactic CR production depending on progenitor masses.

We use RATPaC and PLUTO to simultaneously solve with spherical symmetry the hydrodynamic equations, the transport equations for CRs and scattering magnetic turbulence, and the induction equation for the large-scale magnetic field.

Our study shows a significant impact of the hot wind material. For example, the hot shocked wind created by $60\,M_{\odot}$ Wolf-Rayet progenitor significantly reduces the sonic Mach number of that SNR shock and hence persistently softens the particle spectra with spectral index $\sim\,2.5$, specifically at lower energy, and likewise the radio spectra with spectral index $\alpha \sim 0.8$ (energy flux, $S_\nu \propto \nu^{-\alpha}$).
In contrast, the SNR with $20\,M_{\odot}$ Red-Super giant (RSG) progenitor produces soft radio spectra with spectral index $\sim\,2.2$, and correspondingly soft pion-decay gamma-ray spectra, only briefly during the interaction of the SNR shock with the dense RSG shell. For old remnants with shocks inside the shocked interstellar medium, we find soft pion-decay emission for all progenitors, consistent with the observed gamma-ray emission from SNRs like IC443, W44, G$39.2$-$0.3$, etc.

The flux of CRs released into the interstellar medium is the highest for low-mass progenitors that are in the RSG phase in the pre-supernova stage. The total production spectrum of
cosmic rays injected into the interstellar medium from remnants with $35\,M_\odot$ progenitor has a spectral index of $s\sim2.4$ at higher energies which is comparable with the spectra predicted by Galactic propagation models.