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Pre-explosive accretion and simmering phases of Type Ia Supernovae by Piersanti, Luciano; Bravo, Eduardo; Straniero, Oscar; Cristallo, Sergio; Dominguez, Inmaculada is a scholarly article available to read on EtoBox.

What is Pre-explosive accretion and simmering phases of Type Ia Supernovae about?

In accreting WDs approaching the Chandrasekhar limit, hydrostatic carbon burning precedes the dynamical breakout. During this \textit{simmering} phase, $e-$captures are energetically favored in the central region of the star, while $\beta-$decays are favored more outside, and the two zones are connected by a growing convective instability. We analyze the interplay between weak interactions and convection, the so-called convective URCA process, during the simmering phase of SNe Ia progenitors and its effects on the physical and chemical properties at the explosion epoch. At variance with previous studies, we find that the convective core powered by the carbon burning remains confined within the ${^{21}(Ne,F)}$ URCA shell. As a result, a much larger amount of carbon has to be consumed before the explosion which eventually occurs at larger density than previously estimated. In addition, we find that the extension of the convective core and its average neutronization depend on the the WD progenitor initial metallicity. For the average neutronization in the convective core at the explosion epoch we obtain ${\overline{\eta}_{exp}} = (1.094\pm 0.143)\times 10^{-3} + (9.168\pm 0.677)\times

Author

Piersanti, Luciano; Bravo, Eduardo; Straniero, Oscar; Cristallo, Sergio; Dominguez, Inmaculada

Published

2021

Language

EN