The history of the progenitor supernovae (SNe) plays an important role in the morphology and physical properties of supernova remnants (SNR); the aim of this work is to investigate how the various stellar layers at the time of the explosion map to the resulting abundance pattern observed when the remnant is fully developed. We performed three-dimensional magneto-hydrodynamical simulations starting soon after the core-collapse and following the interaction of the SN ejecta with the circumstellar medium (consisting in the wind of the stellar progenitor), obtaining the physical scenario of a SNR. We investigated how the ejecta distribution of two different progenitors can affect the matter mixing of heavy elements in the remnant from the onset of the SN to 500 years. An 16M-ejecta blue supergiant (BSG) progenitor and a 19M-ejecta red supergiant (RSG) progenitor are investigated. Here we report the preliminary results which show the matter mixing of heavy elements for both SNRs.