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http://hdl.handle.net/10261/340144
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dc.contributor.author | Velilla Prieto, L. | es_ES |
dc.contributor.author | Fonfría, J. P. | es_ES |
dc.contributor.author | Agúndez, Marcelino | es_ES |
dc.contributor.author | Castro-Carrizo, A. | es_ES |
dc.contributor.author | Guélin, M. | es_ES |
dc.contributor.author | Quintana-Lacaci, G. | es_ES |
dc.contributor.author | Cherchneff, I. | es_ES |
dc.contributor.author | Joblin, C. | es_ES |
dc.contributor.author | McCarthy, M. C. | es_ES |
dc.contributor.author | Martín-Gago, José A. | es_ES |
dc.contributor.author | Cernicharo, José | es_ES |
dc.date.accessioned | 2023-12-04T09:54:39Z | - |
dc.date.available | 2023-12-04T09:54:39Z | - |
dc.date.issued | 2023-05-17 | - |
dc.identifier.citation | Nature 617: 696–700 (2023) | es_ES |
dc.identifier.issn | 0028-0836 | - |
dc.identifier.uri | http://hdl.handle.net/10261/340144 | - |
dc.description | 19 pags., 4 + 10 figs. | es_ES |
dc.description.abstract | During their thermally pulsing phase, asymptotic giant branch (AGB) stars eject material that forms extended dusty envelopes1. Visible polarimetric imaging found clumpy dust clouds within two stellar radii of several oxygen-rich stars2-6. Inhomogeneous molecular gas has also been observed in multiple emission lines within several stellar radii of different oxygen-rich stars, including W Hya and Mira7-10. At the stellar surface level, infrared images have shown intricate structures around the carbon semiregular variable R Scl and in the S-type star π1 Gru11,12. Infrared images have also shown clumpy dust structures within a few stellar radii of the prototypical carbon AGB star IRC+10°216 (refs. 13,14), and studies of molecular gas distribution beyond the dust formation zone have also shown complex circumstellar structures15. Because of the lack of sufficient spatial resolution, however, the distribution of molecular gas in the stellar atmosphere and the dust formation zone of AGB carbon stars is not known, nor is how it is subsequently expelled. Here we report observations with a resolution of one stellar radius of the recently formed dust and molecular gas in the atmosphere of IRC+10°216. Lines of HCN, SiS and SiC2 appear at different radii and in different clumps, which we interpret as large convective cells in the photosphere, as seen in Betelgeuse16. The convective cells coalesce with pulsation, causing anisotropies that, together with companions17,18, shape its circumstellar envelope. | es_ES |
dc.description.sponsorship | This publication is part of project ‘I+D+i’ (research, development and innovation, nos. PID2020-117034RJ-I00, PID2019-107115GB-C21, PID2019-106110GB-I00 and PID2019-105203GB-C22) supported by the Spanish Ministerio de Ciencia e Innovación (MCIN/ AEI/10.13039/501100011033). This work was also supported by the European Research Council under Synergy Grant ERC-2013-SyG, G.A. 610256 (NANOCOSMOS). This work is based on observations carried out with the IRAM, SMA and ALMA telescopes. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). SMA is a joint project between the Smithsonian Astrophysical Observatory (USA) and the Academia Sinica Institute of Astronomy and Astrophysics (Taiwan) and is funded by the Smithsonian Institution and Academia Sinica. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.01215.S, ADS/JAO. ALMA#2013.1.00432.S and ADS/JAO.ALMA#2018.1.01485. ALMA is a partnership that includes ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We made use of CASA software (https://casa.nrao.edu/). The GILDAS package was used to reduce and analyse data (https://www.iram.fr/IRAMFR/GILDAS). We acknowledge the GILDAS software team, in particular S. Bardeau, for their help and assistance. We also thank IRAM staff, who provided relevant information for flux calibration from the Northern Extended Millimetre Array observatory database. | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | Nature Publishing Group | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-117034RJ-I00/ES/QUIMICA EN LAS ENVOLTURAS DE ESTRELLAS POST-AGB/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-107115GB-C21/ES/MOLECULAS COMO PRECURSORES DE LOS GRANOS DE POLVO EN ESTRELLAS EVOLUCIONADAS. DESDE LAS ENVOLTURAS CIRCUNESTELARES AL MEDIO INTERESTELAR/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-106110GB-I00/ES/FEEDBACK Y QUIMICA EN EL MEDIO INTERESTELAR. MODELOS E IMAGENES ESPECTROSCOPICAS CON JWST, SOFIA, IRAM-30M, Y ALMA/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-105203GB-C22/ES/GENESIS DE NEBULOSAS PLANETARIAS: VIENTOS, PERDIDA DE MASA Y LANZAMIENTO DE JETS/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/EC/FP7610256 | es_ES |
dc.relation.ispartof | Nature | es_ES |
dc.relation.isversionof | Postprint | es_ES |
dc.rights | closedAccess | es_ES |
dc.title | Atmospheric molecular blobs shape up circumstellar envelopes of AGB stars | es_ES |
dc.type | artículo | es_ES |
dc.identifier.doi | 10.1038/s41586-023-05917-9 | - |
dc.description.peerreviewed | Peer reviewed | es_ES |
dc.relation.publisherversion | https://doi.org/10.1038/s41586-023-05917-9 | es_ES |
dc.contributor.funder | Ministerio de Ciencia e Innovación (España) | es_ES |
dc.contributor.funder | European Commission | es_ES |
dc.contributor.funder | Centre National de la Recherche Scientifique (France) | es_ES |
dc.contributor.funder | Max Planck Society | es_ES |
dc.contributor.funder | Instituto Geográfico Nacional (España) | es_ES |
dc.contributor.funder | Academia Sinica (Taiwan) | es_ES |
dc.relation.csic | Sí | es_ES |
oprm.item.hasRevision | no ko 0 false | * |
dc.identifier.funder | http://dx.doi.org/10.13039/501100004837 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100001869 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100004794 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100000780 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100004189 | es_ES |
dc.contributor.orcid | Velilla Prieto, L. [0000-0001-8275-9341] | es_ES |
dc.contributor.orcid | Fonfría, J. P. [0000-0002-6556-6692] | es_ES |
dc.contributor.orcid | Quintana-Lacaci, G. [0000-0002-5417-1943] | es_ES |
dc.contributor.orcid | Joblin, C. [0000-0003-1561-6118] | es_ES |
dc.contributor.orcid | Martín-Gago, J. A. [0000-0003-2663-491X] | es_ES |
dc.contributor.orcid | Cernicharo, José [0000-0002-3518-2524] | es_ES |
dc.identifier.pmid | 37198489 | - |
dc.identifier.scopus | 2-s2.0-85159432226 | - |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/85159432226 | - |
dc.type.coar | http://purl.org/coar/resource_type/c_6501 | es_ES |
item.cerifentitytype | Publications | - |
item.languageiso639-1 | en | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.grantfulltext | none | - |
item.fulltext | No Fulltext | - |
item.openairetype | artículo | - |
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