Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32970
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Eduardo Bravo | en_US |
dc.contributor.author | Luciano Piersanti | en_US |
dc.contributor.author | Stéphane Blondin | en_US |
dc.contributor.author | Inma Domínguez | en_US |
dc.contributor.author | Oscar Straniero | en_US |
dc.contributor.author | CRISTALLO, Sergio | en_US |
dc.date.accessioned | 2023-01-20T16:10:00Z | - |
dc.date.available | 2023-01-20T16:10:00Z | - |
dc.date.issued | 2022 | en_US |
dc.identifier.issn | 1745-3925 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32970 | - |
dc.description.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. | en_US |
dc.language.iso | eng | en_US |
dc.title | Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnrasl/slac103 | en_US |
dc.identifier.url | http://arxiv.org/abs/2209.04020v1 | en_US |
dc.identifier.url | https://academic.oup.com/mnrasl/article-abstract/517/1/L31/6694255 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 517 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | L31 | en_US |
dc.relation.lastpage | L35 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | ESP | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. LETTERS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Abruzzo | - |
crisitem.author.orcid | 0000-0001-9683-9406 | - |
crisitem.journal.journalissn | 1745-3925 | - |
crisitem.journal.ance | E205843 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
Bravo_2022_MNRAS_517_L31.pdf | PDF editoriale | 656.97 kB | Adobe PDF | View/Open |
Page view(s)
21
checked on May 21, 2024
Download(s)
4
checked on May 21, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.