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dc.contributor.authorQuintana Rodríguez, Carmen-
dc.contributor.authorAgúndez, Marcelino-
dc.contributor.authorCernicharo, José-
dc.contributor.authorBujarrabal, V.-
dc.contributor.authorSánchez Contreras, C.-
dc.contributor.authorCastro-Carrizo, A.-
dc.contributor.authorAlcolea, J.-
dc.date.accessioned2019-07-11T10:40:16Z-
dc.date.available2019-07-11T10:40:16Z-
dc.date.issued2016-07-22-
dc.identifierdoi: 10.1051/0004-6361/201527688-
dc.identifiere-issn: 1432-0746-
dc.identifierissn: 0004-6361-
dc.identifier.citationAstronomy and Astrophysics 592: A51 (2016)-
dc.identifier.urihttp://hdl.handle.net/10261/185935-
dc.description.abstract[Aims] Our knowledge of the chemical properties of the circumstellar ejecta of the most massive evolved stars is particularly poor. We aim to study the chemical characteristics of the prototypical yellow hypergiant star, IRC +10420. For this purpose, we obtained full line surveys at 1 and 3 mm atmospheric windows.-
dc.description.abstract[Methods] We have identified 106 molecular emission lines from 22 molecular species. Approximately half of the molecules detected are N-bearing species, in particular HCN, HNC, CN, NO, NS, PN, and NH. We used rotational diagrams to derive the density and rotational temperature of the different molecular species detected. We introduced an iterative method that allows us to take moderate line opacities into account.-
dc.description.abstract[Results] We have found that IRC +10420 presents high abundances of the N-bearing molecules compared with O-rich evolved stars. This result supports the presence of a N-rich chemistry, expected for massive stars. Our analysis also suggests a decrease of the C/C ratio from ≳ 7 to ∼3.7 in the last 3800 yr, which can be directly related to the nitrogen enrichment observed. In addition, we found that SiO emission presents a significant intensity decrease for high-J lines when compared with older observations. Radiative transfer modeling shows that this variation can be explained by a decrease in the infrared (IR) flux of the dust. The origin of this decrease might be an expansion of the dust shell or a lower stellar temperature due to the pulsation of the star.-
dc.description.sponsorshipThe research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007−2013)/ERC Grant Agreement n. 610256 (NANOCOSMOS). We would also like to thank the Spanish MINECO for funding support from grants CSD2009-00038, AYA2009-07304 and AYA2012-32032.-
dc.publisherEDP Sciences-
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/610256-
dc.rightsclosedAccess-
dc.subjectStars: individual: IRC +10420-
dc.subjectMolecular processes-
dc.subjectCircumstellar matter-
dc.subjectRadio lines: stars-
dc.titleA λ 3 mm and 1 mm line survey toward the yellow hypergiant IRC +10420: N-rich chemistry and IR flux variations-
dc.typeartículo-
dc.identifier.doihttp://dx.doi.org/10.1051/0004-6361/201527688-
dc.relation.publisherversionhttps://doi.org/10.1051/0004-6361/201527688-
dc.date.updated2019-07-11T10:40:16Z-
dc.language.rfc3066eng-
dc.contributor.funderMinisterio de Ciencia e Innovación (España)-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderEuropean Research Council-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004837es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
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