Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27823
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Colzi, L. | en_US |
dc.contributor.author | FONTANI, FRANCESCO | en_US |
dc.contributor.author | Caselli, P. | en_US |
dc.contributor.author | Ceccarelli, C. | en_US |
dc.contributor.author | Hily-Blant, P. | en_US |
dc.contributor.author | Bizzocchi, L. | en_US |
dc.date.accessioned | 2020-10-14T15:05:47Z | - |
dc.date.available | 2020-10-14T15:05:47Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27823 | - |
dc.description.abstract | The ratio between the two stable isotopes of nitrogen, <SUP>14</SUP>N and <SUP>15</SUP>N, is well measured in the terrestrial atmosphere ( 272), and for the pre-solar nebula ( 441, deduced from the solar wind). Interestingly, some pristine solar system materials show enrichments in <SUP>15</SUP>N with respect to the pre-solar nebula value. However, it is not yet clear if and how these enrichments are linked to the past chemical history because we have only a limited number of measurements in dense star-forming regions. In this respect, dense cores, which are believed to be the precursors of clusters and also contain intermediate- and high-mass stars, are important targets because the solar system was probably born within a rich stellar cluster, and such clusters are formed in high-mass star-forming regions. The number of observations in such high-mass dense cores has remained limited so far. In this work, we show the results of IRAM-30 m observations of the J = 1-0 rotational transition of the molecules HCN and HNC and their <SUP>15</SUP>N-bearing counterparts towards 27 intermediate- and high-mass dense cores that are divided almost equally into three evolutionary categories: high-mass starless cores, high-mass protostellar objects, and ultra-compact HII regions. We have also observed the DNC(2-1) rotational transition in order to search for a relation between the isotopic ratios D/H and <SUP>14</SUP>N/<SUP>15</SUP>N. We derive average <SUP>14</SUP>N/<SUP>15</SUP>N ratios of 359 ± 16 in HCN and of 438 ± 21 in HNC, with a dispersion of about 150-200. We find no trend of the <SUP>14</SUP>N/<SUP>15</SUP>N ratio with evolutionary stage. This result agrees with what has been found for N<SUB>2</SUB>H<SUP>+</SUP> and its isotopologues in the same sources, although the <SUP>14</SUP>N/<SUP>15</SUP>N ratios from N<SUB>2</SUB>H<SUP>+</SUP> show a higher dispersion than in HCN/HNC, and on average, their uncertainties are larger as well. Moreover, we have found no correlation between D/H and <SUP>14</SUP>N/<SUP>15</SUP>N in HNC. These findings indicate that (1) the chemical evolution does not seem to play a role in the fractionation of nitrogen, and that (2) the fractionation of hydrogen and nitrogen in these objects is not related. <P />IRAM data used in the paper (FITS) is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A129">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A129 | en_US |
dc.language.iso | eng | en_US |
dc.title | Nitrogen and hydrogen fractionation in high-mass star-forming cores from observations of HCN and HNC | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201730576 | en_US |
dc.identifier.scopus | 2-s2.0-85041387397 | en_US |
dc.identifier.isi | 000429205200001 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2018/01/aa30576-17/aa30576-17.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 609 | en_US |
dc.relation.firstpage | A129 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 6 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018A&A...609A.129C | 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.grantfulltext | open | - |
item.cerifentitytype | Publications | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0003-0348-3418 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
---|---|---|---|---|
aa30576-17.pdf | Pdf editoriale | 802.93 kB | Adobe PDF | Visualizza/apri |
1709.04237.pdf | postprint | 819.3 kB | Adobe PDF | Visualizza/apri |
Page view(s)
41
controllato il 1-set-2024
Download(s)
26
controllato il 1-set-2024
Google ScholarTM
Check
Altmetric
Altmetric
Tutti i documenti in DSpace sono pubblicati ad Accesso Aperto, salvo diversa indicazione per alcuni documenti specifici.