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The aim of this work is to bridge the gap between CC SNe and their remnantsby investigating how post-explosion anisotropies in the ejecta influence thestructure and chemical properties of the remnant at later times. We performedthree-dimensional magneto-hydrodynamical simulations starting soon after the SNevent and following the evolution of the system in the circumstellar medium(consisting of the wind of the stellar progenitor), for 5000 years, obtainingthe physical scenario of a SNR. Here we focused the analysis on the case of aprogenitor red supergiant of 19.8 M_sun. We also investigated how apost-explosion large-scale anisotropy in the SN affects the ejecta distributionand the matter mixing of heavy elements in the remnant, during the first 5000years of evolution. In the case of a spherically symmetric SN explosion withoutlarge-scale anisotropies, the remnant roughly keeps memory of the originalonion-like layering of ejecta soon after the SN event. Nevertheless, as thereverse shock hits the ejecta, the element distribution departs from ahomologous expansion, because of the slowing down of the outermost ejectalayers due to interaction with the reverse shock. In the case of a large-scaleanisotropy developed after the SN, we found that the chemical stratification inthe ejecta can be strongly modified and the original onion-like layering is notpreserved. The anisotropy may cause spatial inversion of ejecta layers, forinstance leading to Fe/Si-rich ejecta outside the O shell, and may determinethe formation of Fe/Si-rich jet-like features that may protrude the remnantoutline. The level of matter mixing and the properties of the jet-like featureare sensitive to the initial physical (density and velocity) and geometrical(size and position) initial characteristics of the anisotropy.

3D modeling from the onset of the SN to the full-fledged SNR: Role of an initial ejecta anisotropy on matter mixing