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One of the key observables for determining the progenitor nature of Type Iasupernovae is provided by their immediate circumstellar medium, which accordingto several models should be shaped by the progenitor binary system. So far,X-ray and radio observations indicate that the surroundings are very tenuous,producing severe upper-limits on the mass loss from winds of the progenitors.In this study, we perform numerical hydro-dynamical simulations of theinteraction of the SN ejecta with circumstellar structures formed by possiblemass outflows from the progenitor systems and we estimate numerically theexpected numerical X-ray luminosity. We consider two kinds of circumstellarstructures: a) A circumstellar medium formed by the donor star's stellar wind,in case of a symbiotic binary progenitor system; b) A circumstellar mediumshaped by the interaction of the slow wind of the donor star with consecutivenova outbursts for the case of a symbiotic recurrent nova progenitor system.For the hydro-simulations we used well-known Type Ia supernova explosionmodels, as well as an approximation based on a power law model for the densitystructure of the outer ejecta. We confirm the strict upper limits on stellarwind mass loss, provided by simplified interpretations of X-ray upper limits ofType Ia supernovae. However, we show that supernova explosions going off in thecavities created by repeated nova explosions, provide a possible explanationfor the lack of X-ray emission from supernovae originating from symbioticbinaries. Moreover, the velocity structure of circumstellar medium, shaped by aseries of nova explosion matches well with the Na absorption features seen inabsorption toward several Type Ia supernovae.

Early X-ray emission from Type Ia supernovae originating from symbiotic progenitors or recurrent novae