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dc.contributor.authorJuhász, Attila
dc.contributor.authorDullemond, Cornelis P.
dc.contributor.authorVan Boekel, Roy
dc.contributor.authorBouwman, Jeroen
dc.contributor.authorÁbrahám, Péter
dc.contributor.authorAcosta-Pulido, José Antonio
dc.contributor.authorKóspál, Ågnes
dc.contributor.authorSicilia-Aguilar, Aurora
dc.contributor.authorJones, Anthony P.
dc.contributor.authorMoór, Attila
dc.contributor.authorMosoni, László
dc.contributor.authorRegály, Zs
dc.contributor.authorSzokoly, Gyula P.
dc.contributor.authorSipos, Nikoletta
dc.contributor.authorHenning, Th.
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2014-10-06T11:21:25Z
dc.date.available2014-10-06T11:21:25Z
dc.date.issued2012-01-10
dc.identifier.citationThe Astrophysical Journal 744.2 (2012): 118en_US
dc.identifier.issn0004-637X (print)es_ES
dc.identifier.issn1538-4357 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/662066
dc.descriptionThe Astrophysical Journal 744.2 (2012): 118 reproduced by permission of the AASen_US
dc.description.abstractEXLup is the prototype of the EXor class of eruptive young stars. These objects show optical outbursts which are thought to be related to runaway accretion onto the star. In a previous study we observed in situ crystal formation in the disk of EXLup during its latest outburst in 2008, making the object an ideal laboratory to investigate circumstellar crystal formation and transport. This outburst was monitored by a campaign of ground-based and Spitzer Space Telescope observations. Here we modeled the spectral energy distribution (SED) of EXLup in the outburst from optical to millimeter wavelengths with a two-dimensional radiative transfer code. Our results showed that the shape of the SED at optical wavelengths was more consistent with a single-temperature blackbody than a temperature distribution. We also found that this single-temperature component emitted 80%-100% of the total accretion luminosity. We concluded that a thermal instability, the most widely accepted model of EXor outbursts, was likely not the triggering mechanism of the 2008 outburst of EXLup. Our mid-infrared Spitzer spectra revealed that the strength of all crystalline bands between 8 and 30μm increased right after the end of the outburst. Six months later, however, the crystallinity in the 10μm silicate feature complex decreased. Our modeling of the mid-infrared spectral evolution of EXLup showed that, although vertical mixing should be stronger during the outburst than in the quiescent phase, fast radial transport of crystals (e.g., by stellar/disk wind) was required to reproduce the observed mid-infrared spectra.en_US
dc.description.sponsorshipThe research of A.K. is supported by the Netherlands Organization for Scientific Research. The research of Zs.R. is supported by the “Lendület” Young Researcher Program of the Hungarian Academy of Sciences.en_US
dc.format.extent15 pag.es_ES
dc.format.mimetypeapplication/pdfen
dc.language.isoengen
dc.publisherThe American Astronomical Society.en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rights© 2012 The American Astronomical Society.en_US
dc.subject.otherAccretionen_US
dc.subject.otherAccretion disksen_US
dc.subject.otherAstrochemistryen_US
dc.subject.otherCircumstellar matteren_US
dc.subject.otherInfrared: starsen_US
dc.subject.otherProtoplanetary disksen_US
dc.subject.otherStars: formationen_US
dc.subject.otherStars: individual (EX Lup)en_US
dc.titleThe 2008 outburst of EX Lup-Silicate crystals in motionen_US
dc.typearticleen
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1088/0004-637X/744/2/118es_ES
dc.identifier.doi10.1088/0004-637X/744/2/118es_ES
dc.identifier.publicationfirstpage118es_ES
dc.identifier.publicationissue2es_ES
dc.identifier.publicationlastpageundefinedes_ES
dc.identifier.publicationvolume744es_ES
dc.type.versioninfo:eu-repo/semantics/publishedVersiones_ES
dc.rights.accessRightsopenAccessen
dc.authorUAMSicilia Aguilar, María De La Aurora (264647)
dc.facultadUAMFacultad de Ciencias


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