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Unveiling the Dust Nucleation Zone of IRC+10216 with ALMA

hal.structure.identifierCentro de Astrobiologia [Madrid] [CAB]
dc.contributor.authorCERNICHARO, J.
dc.contributor.authorDANIEL, F.
dc.contributor.authorCASTRO-CARRIZO, A.
hal.structure.identifierSSE 2013
dc.contributor.authorAGÚNDEZ, M.
dc.contributor.authorMARCELINO, N.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorJOBLIN, C.
hal.structure.identifierCentro de Astrobiologia [Madrid] [CAB]
dc.contributor.authorGOICOECHEA, J. R.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGUÉLIN, M.
dc.date.created2013-10-28
dc.date.issued2013-12
dc.identifier.issn2041-8205
dc.description.abstractEnWe report the detection in IRC+10216 of lines of HNC J = 3 - 2 pertaining to nine excited vibrational states with energies up to ~5300 K. The spectrum, observed with ALMA, also shows a surprising large number of narrow, unidentified lines that arise in the vicinity of the star. The HNC data are interpreted through a 1D-spherical non-local radiative transfer model, coupled to a chemical model that includes chemistry at thermochemical equilibrium for the innermost regions and reaction kinetics for the external envelope. Although unresolved by the current early ALMA data, the radius inferred for the emitting region is ~0.''06 (i.e., ~= 3 stellar radii), similar to the size of the dusty clumps reported by IR studies of the innermost region (r < 0.''3). The derived abundance of HNC relative to H2 is 10-8 < χ(HNC) <10-6, and drops quickly where the gas density decreases and the gas chemistry is dominated by reaction kinetics. Merging HNC data with that of molecular species present throughout the inner envelope, such as vibrationally excited HCN, SiS, CS, or SiO, should allow us to characterize the physical and chemical conditions in the dust formation zone.
dc.language.isoen
dc.publisherBristol : IOP Publishing
dc.title.enUnveiling the Dust Nucleation Zone of IRC+10216 with ALMA
dc.typeArticle de revue
dc.identifier.doi10.1088/2041-8205/778/2/L25
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1310.7383
bordeaux.journalThe Astrophysical journal letters
bordeaux.pageL25
bordeaux.volume778
bordeaux.peerReviewedoui
hal.identifierhal-01016713
hal.version1
hal.popularnon
hal.audienceInternationale
dc.subject.itcircumstellar matter
dc.subject.itline: identification
dc.subject.itmolecular processes
dc.subject.itstars: AGB and post-AGB
dc.subject.itstars: individual: IRC +10216
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01016713v1
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