Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints
Date Issued
2022
Author(s)
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
$(3.6-6.3)\times10^9$ g cm$^{-3}$ 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 ($^{54}$Cr) and titanium ($^{50}$Ti). 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.
Volume
517
Issue
1
Start page
L31
Issn Identifier
1745-3925
Rights
open.access
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