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http://hdl.handle.net/20.500.12386/32970
Title: | Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints | Authors: | Eduardo Bravo Luciano Piersanti Stéphane Blondin Inma Domínguez Oscar Straniero CRISTALLO, Sergio |
Issue Date: | 2022 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. LETTERS | Number: | 517 | Issue: | 1 | First Page: | L31 | 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. | URI: | http://hdl.handle.net/20.500.12386/32970 | URL: | http://arxiv.org/abs/2209.04020v1 https://academic.oup.com/mnrasl/article-abstract/517/1/L31/6694255 |
ISSN: | 1745-3925 | DOI: | 10.1093/mnrasl/slac103 | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Bravo_2022_MNRAS_517_L31.pdf | PDF editoriale | 656.97 kB | Adobe PDF | View/Open |
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