  The structure and morphology of supernova remnants (SNRs) reflect the
properties of the parent supernovae (SNe) and the characteristics of the
inhomogeneous environments through which the remnants expand. Linking the
morphology of SNRs to anisotropies developed in their parent SNe can be
essential to obtain key information on many aspects of the explosion processes
associated with SNe. Nowadays, our capability to study the SN-SNR connection
has been largely improved thanks to multi-dimensional models describing the
long-term evolution from the SN to the SNR as well as to observational data of
growing quality and quantity across the electromagnetic spectrum which allow to
constrain the models. Here we used the numerical resources obtained in the
framework of the "Accordo Quadro INAF-CINECA (2017)" together with a CINECA
ISCRA Award N.HP10BARP6Y to describe the full evolution of a SNR from the
core-collapse to the full-fledged SNR at the age of 2000 years. Our simulations
were compared with observations of SNR Cassiopeia A (Cas A) at the age of $\sim
350$~years. Thanks to these simulations we were able to link the physical,
chemical and morphological properties of a SNR to the physical processes
governing the complex phases of the SN explosion.
