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http://hdl.handle.net/20.500.12386/23499
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | FONTANI, FRANCESCO | en_US |
dc.contributor.author | Caselli, P. | en_US |
dc.contributor.author | Palau, A. | en_US |
dc.contributor.author | Bizzocchi, L. | en_US |
dc.contributor.author | Ceccarelli, C. | en_US |
dc.date.accessioned | 2020-03-23T17:20:52Z | - |
dc.date.available | 2020-03-23T17:20:52Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 2041-8205 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23499 | - |
dc.description.abstract | We report on the first measurements of the isotopic ratio <SUP>14</SUP>N/<SUP>15</SUP>N in N<SUB>2</SUB>H<SUP>+</SUP> toward a statistically significant sample of high-mass star-forming cores. The sources belong to the three main evolutionary categories of the high-mass star formation process: high-mass starless cores, high-mass protostellar objects, and ultracompact H ii regions. Simultaneous measurements of the <SUP>14</SUP>N/<SUP>15</SUP>N ratio in CN have been made. The <SUP>14</SUP>N/<SUP>15</SUP>N ratios derived from N<SUB>2</SUB>H<SUP>+</SUP> show a large spread (from ∼180 up to ∼1300), while those derived from CN are in between the value measured in the terrestrial atmosphere (∼270) and that of the proto-solar nebula (∼440) for the large majority of the sources within the errors. However, this different spread might be due to the fact that the sources detected in the N<SUB>2</SUB>H<SUP>+</SUP> isotopologues are more than those detected in the CN ones. The <SUP>14</SUP>N/<SUP>15</SUP>N ratio does not change significantly with the source evolutionary stage, which indicates that time seems to be irrelevant for the fractionation of nitrogen. We also find a possible anticorrelation between the <SUP>14</SUP>N/<SUP>15</SUP>N (as derived from N<SUB>2</SUB>H<SUP>+</SUP>) and the H/D isotopic ratios. This suggests that <SUP>15</SUP>N enrichment could not be linked to the parameters that cause D enrichment, in agreement with the prediction by recent chemical models. These models, however, are not able to reproduce the observed large spread in <SUP>14</SUP>N/<SUP>15</SUP>N, pointing out that some important routes of nitrogen fractionation could be still missing in the models. <P />Based on observations carried out with the IRAM-30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). | en_US |
dc.language.iso | eng | en_US |
dc.title | First Measurements of <SUP>15</SUP>N Fractionation in N<SUB>2</SUB>H<SUP>+</SUP> toward High-mass Star-forming Cores | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/2041-8205/808/2/L46 | en_US |
dc.identifier.scopus | 2-s2.0-84938813223 | en_US |
dc.identifier.isi | 000358938800014 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/2041-8205/808/2/L46 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 808 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | L46 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL LETTERS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015ApJ...808L..46F | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò 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.orcid | 0000-0003-0348-3418 | - |
crisitem.journal.journalissn | 2041-8205 | - |
crisitem.journal.ance | E196528 | - |
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