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Chemistry in Disks VIII: the CS molecule as an analytic tracer of turbulence in disks

hal.structure.identifierAMOR 2012
dc.contributor.authorGUILLOTEAU, S.
hal.structure.identifierAMOR 2012
dc.contributor.authorDUTREY, Anne
hal.structure.identifierAMOR 2012
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERSANT, F.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorSEMENOV, D.
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierAMOR 2012
dc.contributor.authorCHAPILLON, E.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, T.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorPIÉTU, V.
dc.date.created2012-11-21
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnTurbulence is thought to be a key driver of the evolution of protoplanetary disks, regulating the mass accretion process, the transport of angular momentum, and the growth of dust particles. We intend to determine the magnitude of the turbulent motions in the outer parts (> 100 AU) of the disk surrounding DM Tau. Turbulent motions can be constrained by measuring the nonthermal broadening of line emission from heavy molecules. We used the IRAM Plateau de Bure interferometer to study emission from the CS molecule in the disk of DM Tau. High spatial (1.4 x 1 ") and spectral resolution (0.126 km/s) CS J=3-2 images provide constraints on the molecule distribution and velocity structure of the disk. A low sensitivity CS J=5-4 image was used in conjunction to evaluate the excitation conditions. We analyzed the data in terms of two parametric disk models, and compared the results with detailed time-dependent chemical simulations. The CS data confirm the relatively low temperature suggested by observations of other simple molecules. The intrinsic linewidth derived from the CS J=3-2 data is much larger than expected from pure thermal broadening. The magnitude of the derived nonthermal component depends only weakly on assumptions about the location of the CS molecules with respect to the disk plane. Our results indicate turbulence with a Mach number around 0.4 - 0.5 in the molecular layer. Geometrical constraints suggest that this layer is located near one scale height, in reasonable agreement with chemical model predictions.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enprotoplanetary disks
dc.subject.enradio lines: planetary systems
dc.subject.enradio lines: stars
dc.subject.encircumstellar matter
dc.title.enChemistry in Disks VIII: the CS molecule as an analytic tracer of turbulence in disks
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201220331
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1211.4969
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A70
bordeaux.volume548
bordeaux.peerReviewedoui
hal.identifierhal-00764159
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00764159v1
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