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The study of core-collapse supernova remnants (SNRs) presents a fascinatingpuzzle, with intricate morphologies and a non-uniform distribution of stellardebris. Particularly, young remnants (aged less than 5000 years) hold immensevalue as they can offer crucial insights into the inner processes of thesupernova (SN) engine, revealing details about nucleosynthetic yields andlarge-scale asymmetries arising from the early stages of the explosion.Furthermore, these remnants also bear characteristics that may reflect thenature of their progenitor stars and the interactions between the remnants andthe surrounding circumstellar medium (CSM), shaped by the progenitor'smass-loss history. Hence, investigating the connection between young SNRs,parent SNe, and progenitor massive stars can be of paramount importance todelve into the physics of SN engines, and to investigate the final stages ofmassive star evolution and the elusive mechanisms governing their mass loss. Inthis contribution, I review recent advances in modeling the path from massivestars to SNe and SNRs achieved by our team. The focus is on investigating thelinks between the observed physical and chemical properties of SNRs and theirprogenitor stars and SN explosions. The unraveling of this connection offers usthe opportunity to probe the physics of core-collapse SN explosions and thefinal stages of evolution of massive stars.

Modeling the Evolution from Massive Stars to Supernovae and Supernova Remnants