Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26807
DC Field | Value | Language |
---|---|---|
dc.contributor.author | CHIEFFI, ALESSANDRO | en_US |
dc.contributor.author | LIMONGI, Marco | en_US |
dc.date.accessioned | 2020-08-25T13:56:47Z | - |
dc.date.available | 2020-08-25T13:56:47Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26807 | - |
dc.description.abstract | We discuss the influence of rotation on the combined synthesis of {}<SUP>44</SUP>{Ti} and {}<SUP>56</SUP>{Ni} in massive stars. While {}<SUP>56</SUP>{Ni} is significantly produced by both complete and incomplete explosive Si burning, {}<SUP>44</SUP>{Ti} is mainly produced by complete explosive Si burning, with a minor contribution (in standard non-rotating models) from incomplete explosive Si burning and O burning (both explosive and hydrostatic). We find that, in most cases, the thickness of the region exposed to incomplete explosive Si burning increases in rotating models (initial velocity, v <SUB>ini</SUB> = 300 km s<SUP>-1</SUP>) and since {}<SUP>56</SUP>{Ni} is significantly produced in this zone, the fraction of mass coming from the complete explosive Si burning zone necessary to get the required amount of {}<SUP>56</SUP>{Ni} reduces. Therefore the amount of {}<SUP>44</SUP>{Ti} ejected for a given fixed amount of {}<SUP>56</SUP>{Ni} decreases in rotating models. However, some rotating models at [Fe/H] = -1 develop a very extended O convective shell in which a consistent amount of {}<SUP>44</SUP>{Ti} is formed, preserved, and ejected in the interstellar medium. Hence a better modeling of the thermal instabilities (convection) in the advanced burning phases together with a critical analysis of the cross sections of the nuclear reactions operating in O burning are relevant for the understanding of the synthesis of {}<SUP>44</SUP>{Ti}. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Synthesis of 44 Ti and 56 Ni in Massive Stars | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/836/1/79 | en_US |
dc.identifier.scopus | 2-s2.0-85014312290 | en_US |
dc.identifier.isi | 000397304500031 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/836/1/79 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 836 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 79 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 2 | en_US |
dc.description.international | no | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017ApJ...836...79C | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | sì | 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. Roma | - |
crisitem.author.orcid | 0000-0002-3589-3203 | - |
crisitem.author.orcid | 0000-0003-0636-7834 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Chieffi_2017_ApJ_836_79.pdf | 497.09 kB | Adobe PDF | View/Open | |
1701.02914.pdf | 236.41 kB | Adobe PDF | View/Open |
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