Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27808
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Colzi, L. | en_US |
dc.contributor.author | FONTANI, FRANCESCO | en_US |
dc.contributor.author | RIVILLA RODRIGUEZ, VICTOR MANUEL | en_US |
dc.contributor.author | Sánchez-Monge, A. | en_US |
dc.contributor.author | TESTI, Leonardo | en_US |
dc.contributor.author | BELTRAN SOROLLA, MARIA TERESA | en_US |
dc.contributor.author | Caselli, P. | en_US |
dc.date.accessioned | 2020-10-14T14:12:39Z | - |
dc.date.available | 2020-10-14T14:12:39Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27808 | - |
dc.description.abstract | The fractionation of nitrogen (N) in star-forming regions is a poorly understood process. To put more stringent observational constraints on the N-fractionation, we have observed with the IRAM-30-m telescope a large sample of 66 cores in massive star-forming regions. We targeted the (1-0) rotational transition of HN<SUP>13</SUP>C, HC<SUP>15</SUP>N, H<SUP>13</SUP>CN and HC<SUP>15</SUP>N, and derived the <SUP>14</SUP>N/<SUP>15</SUP>N ratio for both HCN and HNC. We have completed this sample with that already observed by Colzi et al., and thus analysed a total sample of 87 sources. The <SUP>14</SUP>N/<SUP>15</SUP>N ratios are distributed around the Proto-Solar Nebula value with a lower limit near the TA value (∼272). We have also derived the <SUP>14</SUP>N/<SUP>15</SUP>N ratio as a function of the Galactocentric distance and deduced a linear trend based on unprecedented statistics. The Galactocentric dependences that we have found are consistent, in the slope, with past works but we have found a new local <SUP>14</SUP>N/<SUP>15</SUP>N value of ∼400, i.e. closer to the Prosolar Nebula value. A second analysis was done, and a parabolic Galactocentric trend was found. Comparison with Galactic chemical evolution models shows that the slope until 8 kpc is consistent with the linear analysis, while the flattening trend above 8 kpc is well reproduced by the parabolic analysis. | en_US |
dc.language.iso | eng | en_US |
dc.title | Nitrogen fractionation in high-mass star-forming cores across the Galaxy | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty1027 | en_US |
dc.identifier.scopus | 2-s2.0-85053539626 | en_US |
dc.identifier.isi | 000441282300062 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/478/3/3693/4983135 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 478 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3693 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 7 | en_US |
dc.description.international | sì | 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 | 2018MNRAS.478.3693C | 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. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0003-0348-3418 | - |
crisitem.author.orcid | 0000-0002-2887-5859 | - |
crisitem.author.orcid | 0000-0003-1859-3070 | - |
crisitem.author.orcid | 0000-0003-3315-5626 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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File | Descrizione | Dimensioni | Formato | |
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sty1027.pdf | Pdf editoriale | 1.8 MB | Adobe PDF | Visualizza/apri |
1804.05717.pdf | postprint | 1.56 MB | Adobe PDF | Visualizza/apri |
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