Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32405
DC Field | Value | Language |
---|---|---|
dc.contributor.author | MOLARO, Paolo | en_US |
dc.contributor.author | Izzo, L. | en_US |
dc.contributor.author | Bonifacio, P. | en_US |
dc.contributor.author | Hernanz, M. | en_US |
dc.contributor.author | Selvelli, P. | en_US |
dc.contributor.author | DELLA VALLE, Massimo | en_US |
dc.date.accessioned | 2022-06-20T09:21:34Z | - |
dc.date.available | 2022-06-20T09:21:34Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32405 | - |
dc.description.abstract | Following the recent detection of <SUP>7</SUP>Be II in the outburst spectra of classical novae, we report the search for this isotope in the outbursts of four recent bright novae by means of high-resolution Ultraviolet and Visual Echelle Spectrograph (UVES) observations. The <SUP>7</SUP>Be II λλ313.0583, 313.1228 nm doublet resonance lines are detected in the high-velocity components of Nova Mus 2018 and ASASSN-18fv during outbursts. However, <SUP>7</SUP>Be II is not detected in ASASSN-17hx and possibly not in Nova Cir 2018, which shows that <SUP>7</SUP>Be is not always ejected in the thermonuclear runaway. Taking into account the <SUP>7</SUP>Be decay, we find X(<SUP>7</SUP>Be)/X(H) ≈ 1.5 × 10<SUP>-5</SUP> and 2.2 × 10<SUP>-5</SUP> in Nova Mus 2018 and ASASSN-18fv, respectively. A value of <SUP>7</SUP>Be/H ≈ 2 × 10<SUP>-5</SUP> is found in five out of the seven extant measurements, and it can be considered as a typical <SUP>7</SUP>Be yield for novae. However, this value is almost one order of magnitude larger than predicted by current theoretical models. We argue that the variety of high <SUP>7</SUP>Be/H abundances could be the result of a higher than solar content of <SUP>3</SUP>He in the donor star. The cases with <SUP>7</SUP>Be not detected might be related to the small mass of the white dwarf (WD) or to relatively little mixing with the core material of the WD. The <SUP>7</SUP>Be/H, or <SUP>7</SUP>Li/H, abundance is ≈ 4 dex above meteoritic abundance, thus confirming the novae as the main sources of <SUP>7</SUP>Li in the Milky Way. | en_US |
dc.language.iso | eng | en_US |
dc.title | Search for 7Be in the outbursts of four recent novae | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stz3587 | en_US |
dc.identifier.scopus | 2-s2.0-85087285038 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/492/4/4975/5727881?login=true | en_US |
dc.identifier.url | http://arxiv.org/abs/1912.13281v1 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 492 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 4975 | en_US |
dc.relation.lastpage | 4985 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2020MNRAS.492.4975M | en_US |
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. Trieste | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.orcid | 0000-0002-0571-4163 | - |
crisitem.author.orcid | 0000-0003-3142-5020 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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stz3587.pdf | Pdf editoriale | 2.67 MB | Adobe PDF | View/Open |
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