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The massive protostar W43-MM1 as seen by Herschel-HIFI water spectra: high turbulence and accretion luminosity

hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorCHAVARRIA, L.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorVAN DER TAK, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
hal.structure.identifierLeiden Observatory [Leiden]
dc.contributor.authorVAN DISHOECK, E. F.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorJACQ, T.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBRAINE, J.
hal.structure.identifierEuropean Southern Observatory [ESO]
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBAUDRY, Alain
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorKRISTENSEN, L.
dc.date.created2012-04-02
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnWe present Herschel/HIFI observations of fourteen water lines in W43-MM1, a massive protostellar object in the luminous star cluster-forming region W43. We analyze the gas dynamics from the line profiles using Herschel-HIFI observations (WISH-KP) of fourteen far-IR water lines (H2O, H217O, H218O), CS(11-10), and C18O(9-8) lines, and using our modeling of the continuum spectral energy distribution. As for lower mass protostellar objects, the molecular line profiles are a mix of emission and absorption, and can be decomposed into 'medium', and 'broad' velocity components. The broad component is the outflow associated with protostars of all masses. Our modeling shows that the remainder of the water profiles can be well fitted by an infalling and passively heated envelope, with highly supersonic turbulence varying from 2.2 km/s in the inner region to 3.5 km/s in the outer envelope. Also, W43-MM1 has a high accretion rate, between 4.0 x 10^{-4} and 4.0 x 10^{-2} \msun /yr, derived from the fast (0.4-2.9 km/s) infall observed. We estimate a lower mass limit of gaseous water of 0.11 \msun and total water luminosity of 1.5 \lsun (in the 14 lines presented here). The central hot core is detected with a water abundance of 1.4 x 10^{-4} while the water abundance for the outer envelope is 8 x10^{-8}. The latter value is higher than in other sources, most likely related to the high turbulence and the micro-shocks created by its dissipation. Examining water lines of various energies, we find that the turbulent velocity increases with the distance to the center. While not in clear disagreement with the competitive accretion scenario, this behavior is predicted by the turbulent core model. Moreover, the estimated accretion rate is high enough to overcome the expected radiation pressure.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enThe massive protostar W43-MM1 as seen by Herschel-HIFI water spectra: high turbulence and accretion luminosity
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201118413
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1204.0397
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA76
bordeaux.volume542
bordeaux.peerReviewedoui
hal.identifierhal-00685395
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00685395v1
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