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The nature of Type Ia Supernova (SN Ia) explosions remains an open issue,with several contending progenitor scenarios actively being considered. Onesuch scenario involves a SN Ia explosion inside a planetary nebula (PN) in theaftermath of a stellar merger triggered by a common envelope (CE) episode. Weexamine this scenario using hydrodynamic and non-equilibrium ionizationsimulations of the interaction between the SN ejecta and the PN cocoon into thesupernova remnant (SNR) phase, focusing on the impact of the delay between theCE episode and the SN explosion. We compare the bulk dynamics and X-ray spectraof our simulated SNRs to the observed properties of known Type Ia SNRs in theMilky Way and the Magellanic Clouds. We conclude that models where the SNexplosion happens in the immediate aftermath of the CE episode (with a delay$\lesssim$1,000 yr) are hard to reconcile with the observations, because theinteraction with the dense PN cocoon results in ionization timescales muchhigher than those found in any known Type Ia SNR. Models with a longer delaybetween the CE episode and the SN explosion ($\sim$10,000 yr) are closer to theobservations, and may be able to explain the bulk properties of some Type IaSNRs.

Do Type Ia Supernovae Explode Inside Planetary Nebulae?