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8F41BAFE-B027-4671-9C42-69BA7047FCFA

Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints

Eduardo Bravo, Luciano Piersanti, Stéphane Blondin, Inma Domínguez, Oscar Straniero, Sergio Cristallo
arXiv:2209.04020

Submitted on 8 September 2022

Abstract

The precise progenitor system of type Ia supernovae (SNe Ia), whether it is a white dwarf (WD) close to the Chandrasekhar limit or substantially less massive, has been a matter of debate for decades. Recent research by our group on the accretion and simmering phases preceding the explosion of a massive WD has shown that the central density at thermal runaway lies in the range (3.66.3)×109 g cm3 for reasonable choices of accretion rate onto the WD and progenitor metallicity. In this work, we have computed one-dimensional simulations of the explosion of such WDs, with special emphasis on the chemical composition of the ejecta, which in all cases is extremely rich in neutronized isotopes of chromium (54Cr) and titanium (50Ti). We show that, in order to reconcile such a nucleosynthesis with the isotopic abundances of the Solar System, Chandrasekhar-mass white dwarfs can account for at most 26 per cent of normal-luminosity SNe Ia, or at most 20 per cent of all SNe Ia.

Preprint

Comment: 5 pages, 1 table, 3 figures; Letter accepted by MNRAS

Subjects: Astrophysics - Solar and Stellar Astrophysics; Astrophysics - High Energy Astrophysical Phenomena

URL: https://arxiv.org/abs/2209.04020