Abstract
One of the key methods for determining the unknown nature of Type Ia supernovae (SNe Ia) is the search for traces of interaction between the SN ejecta and the circumstellar structures at the resulting supernova remnants (SNRs Ia). So far, the observables that we receive from well-studied SNRs Ia cannot be explained self-consistently by any model presented in the literature. In this study, we suggest that the circumstellar medium (CSM) being observed to surround several SNRs Ia was mainly shaped by planetary nebulae (PNe) that originated from one or both progenitor stars. Performing two-dimensional hydrodynamic simulations, we show that the ambient medium shaped by PNe can account for several properties of the CSM that have been found to surround SNe Ia and their remnants. Finally, we model Kepler’s SNR considering that the SN explosion occurred inside a bipolar PN. Our simulations show good agreement with the observed morphological and kinematic properties of Kepler’s SNR. In particular, our model reproduces the current expansion parameter of Kepler’s SNR, the partial interaction of the remnant with a dense CSM at its northern region and finally the existence of two opposite protrusions (‘ears’) at the equatorial plane of the SNR.
Highlights
Thermonuclear or Type Ia supernovae (SNe Ia) is a class of supernovae that results from the thermonuclear combustion of a carbon-oxygen white dwarf (WD), which is destabilized through the interaction with a companion star
planetary nebulae (PNe) are formed in the final stages of low mass stars (M ≤ 8 M ) which end their lives as WDs
Regarding the delay time between the PN formation and the subsequent SN Ia explosion, we present three cases each of which represents a specific state of the circumstellar medium (CSM) around the explosion center: (a) the SN Ia occurs almost simultaneously with the birth of the WD i.e., the τdelay is negligible compared to the dynamical timescale of the surrounding PN
Summary
Thermonuclear or Type Ia supernovae (SNe Ia) is a class of supernovae that results from the thermonuclear combustion of a carbon-oxygen white dwarf (WD), which is destabilized through the interaction with a companion star This interaction could appear either via mass transfer from a non-degenerate donor star (single degenerate scenario, SD) or in a merger event with a degenerate companion (double degenerate scenario, DD). Both scenarios have severe weaknesses and cannot account for all the observed properties of SNe Ia [1]. We model the SNR of Kepler within the framework of the studied model and we show that the interaction of the SN ejecta with a surrounding bipolar PN reproduces the overall morphological and kinematic properties of the remnant
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