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Methanol emission from low mass protostars

hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorMARET, S.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorCECCARELLI, C.
hal.structure.identifierSRON Netherlands Institute for Space Research [SRON]
dc.contributor.authorTIELENS, A. G. G. M.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorCAUX, E.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorLEFLOCH, B.
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorFAURE, A.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
dc.contributor.authorCASTETS, Alain
hal.structure.identifierDepartment of Physics [Durham University]
dc.contributor.authorFLOWER, D. R.
dc.date.created2005
dc.date.issued2005
dc.identifier.issn0004-6361
dc.description.abstractEnWe present observations of methanol lines in a sample of Class 0 low mass protostars. Using a 1-D radiative transfer model, we derive the abundances in the envelopes. In two sources of the sample, the observations can only be reproduced by the model if the methanol abundance is enhanced by about two order of magnitude in the inner hot region of the envelope. Two other sources show similar jumps, although at a lower confidence level. The observations for the other three sources are well reproduced with a constant abundance, but the presence of a jump cannot be ruled out. The observed methanol abundances in the warm gas around low mass protostars are orders of magnitude higher than gas phase chemistry models predict. Hence, in agreement with other evidences, this suggest that the high methanol abundance reflects recent evaporation of ices due to the heating by the newly formed star. The observed abundance ratios of CH3 OH, H2 CO, and CO are in good agreement with grain surface chemistry models. However, the absolute abundances are more difficult to reproduce and may point towards the presence of multiple ice components in these regions.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enISM: abundances
dc.subject.enISM: molecules
dc.subject.enstars: formation
dc.title.enMethanol emission from low mass protostars
dc.typeArticle de revue
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
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.arxivastro-ph/0507172
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page527-538
bordeaux.volume442
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00401891
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00401891v1
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