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http://hdl.handle.net/20.500.12386/26163
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Sugimura, K. | en_US |
dc.contributor.author | Coppola, C. M. | en_US |
dc.contributor.author | Omukai, K. | en_US |
dc.contributor.author | GALLI, Daniele | en_US |
dc.contributor.author | Palla, F. | en_US |
dc.date.accessioned | 2020-06-22T10:13:36Z | - |
dc.date.available | 2020-06-22T10:13:36Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26163 | - |
dc.description.abstract | We investigate the role of the H2+ channel on H2 molecule formation during the collapse of primordial gas clouds immersed in strong radiation fields which are assumed to have the shape of a diluted blackbody spectra with temperature Trad. Since the photodissociation rate of H2+ depends on its level population, we take full account of the vibrationally resolved H2+ kinetics. We find that in clouds under soft but intense radiation fields with spectral temperature Trad ≲ 7000 K, the H2+ channel is the dominant H2 formation process. On the other hand, for harder spectra with Trad ≳ 7000 K, the H- channel takes over H2+ in the production of molecular hydrogen. We calculate the critical radiation intensity needed for supermassive star formation by direct collapse and examine its dependence on the H2+ level population. Under the assumption of local thermodynamic equilibrium (LTE) level population, the critical intensity is underestimated by a factor of a few for soft spectra with Trad ≲ 7000 K. For harder spectra, the value of the critical intensity is not affected by the level population of H2+. This result justifies previous estimates of the critical intensity assuming LTE populations since radiation sources like young and/or metal-poor galaxies are predicted to have rather hard spectra. | en_US |
dc.language.iso | eng | en_US |
dc.title | Role of the H_2^+ channel in the primordial star formation under strong radiation field and the critical intensity for the supermassive star formation | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv2655 | en_US |
dc.identifier.scopus | 2-s2.0-84959577029 | en_US |
dc.identifier.isi | 000368010000054 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/456/1/270/1067842 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 456 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 270 | en_US |
dc.relation.lastpage | 277 | en_US |
dc.relation.numberofpages | 7 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | JPN | 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 | 2016MNRAS.456..270S | 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.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0001-7706-6049 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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sugimura_2016_postprint.pdf | Postprint | 504.29 kB | Adobe PDF | Visualizza/apri |
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