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hal.structure.identifierCentre National de la Recherche Scientifique [CNRS]
hal.structure.identifierUniversité Paris-Saclay
hal.structure.identifierInstitut des Sciences Moléculaires d'Orsay [ISMO]
dc.contributor.authorDARTOIS, E.
hal.structure.identifierPhysique des interactions ioniques et moléculaires [PIIM]
hal.structure.identifierCentre National de la Recherche Scientifique [CNRS]
dc.contributor.authorNOBLE, Jennifer
hal.structure.identifierDipartimento di Chimica "Giacomo Ciamician"
dc.contributor.authorCASELLI, P.
dc.contributor.authorFRASER, H.
dc.contributor.authorJIMÉNEZ-SERRA, I.
dc.contributor.authorMATÉ, B.
dc.contributor.authorMCCLURE, M.
dc.contributor.authorMELNICK, G.
dc.contributor.authorPENDLETON, Y.
hal.structure.identifierNiigata University
dc.contributor.authorSHIMONISHI, T.
hal.structure.identifierNOAA Space Environment Center
dc.contributor.authorSMITH, Z.
dc.contributor.authorSTURM, J.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorTAILLARD, A.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorWAKELAM, V.
dc.contributor.authorBOOGERT, A.
hal.structure.identifierUniversität Bern = University of Bern = Université de Berne [UNIBE]
dc.contributor.authorDROZDOVSKAYA, M.
dc.contributor.authorERKAL, J.
dc.contributor.authorHARSONO, D.
dc.contributor.authorHERRERO, V.
hal.structure.identifierQueen Mary University of London [QMUL]
dc.contributor.authorIOPPOLO, S.
hal.structure.identifierLaboratory for Astrophysics
dc.contributor.authorLINNARTZ, H.
hal.structure.identifierDepartment of Chemistry [MIT Cambridge]
hal.structure.identifierNational Radio Astronomy Observatory [Charlottesville] [NRAO]
dc.contributor.authorMCGUIRE, B.
dc.contributor.authorPEROTTI, G.
dc.contributor.authorQASIM, D.
dc.contributor.authorROCHA, W.
dc.date.accessioned2024-11-26T03:25:22Z
dc.date.available2024-11-26T03:25:22Z
dc.date.issued2024-01-09
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/203480
dc.description.abstractEnClouds of gas and dust in the Galaxy are nurseries in which stars and planetary systems are born. Cold dust grains grow icy mantles -by accretion, surface chemistry, and collision mechanisms -during their journey from the diffuse interstellar medium to protoplanetary disks. Our "Ice Age" JWST observations of the dense Chamaeleon I cloud reveal that this growth starts early, before the protostellar phase, significantly modifying the ice absorption band spectroscopic profiles. Spectral analysis confirms that the grains reach micron sizes, implying myriad changes in local microphysics, including mass transfer from small to large grains, reduction in the grain surface available for chemistry, and modification of the penetration and propagation of radiation fields. Deformation of the observed profiles complicates chemical abundance determination. Observing extensive icy growth in dense clouds quantitatively constrains the grain size evolution prior to star-and planet-formation.
dc.language.isoen
dc.publisherNature Publishing Group
dc.subject.enAstrophysical dust
dc.subject.enInterstellar medium
dc.subject.enLaboratory astrophysics
dc.title.enSpectroscopic sizing of interstellar icy grains with JWST
dc.typeArticle de revue
dc.identifier.doi10.1038/s41550-023-02155-x
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.description.sponsorshipEuropeLinking chemistry and physics in the planet-forming zones of disks
bordeaux.journalNature Astronomy
bordeaux.page359-367
bordeaux.volume8
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.issue3
bordeaux.institutionUniversité de Bordeaux
bordeaux.institutionCNRS
bordeaux.peerReviewedoui
hal.identifierhal-04796693
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04796693v1
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