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The precise progenitor system of type Ia supernovae (SNe Ia), whether it is awhite dwarf (WD) close to the Chandrasekhar limit or substantially lessmassive, has been a matter of debate for decades. Recent research by our groupon the accretion and simmering phases preceding the explosion of a massive WDhas 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 ontothe WD and progenitor metallicity. In this work, we have computedone-dimensional simulations of the explosion of such WDs, with special emphasison the chemical composition of the ejecta, which in all cases is extremely richin neutronized isotopes of chromium ($^{54}$Cr) and titanium ($^{50}$Ti). Weshow that, in order to reconcile such a nucleosynthesis with the isotopicabundances of the Solar System, Chandrasekhar-mass white dwarfs can account forat most 26 per cent of normal-luminosity SNe Ia, or at most 20 per cent of allSNe Ia.

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