Ringed Structures of the HD 163296 Protoplanetary Disk Revealed by ALMA

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dc.citation.articleNumber251101
dc.citation.issueNumber25en_US
dc.citation.journalTitlePhysical Review Lettersen_US
dc.citation.volumeNumber114en_US
dc.contributor.authorIsella, Andreaen_US
dc.contributor.authorGuidi, Gretaen_US
dc.contributor.authorTesti, Leonardoen_US
dc.contributor.authorLiu, Shangfeien_US
dc.contributor.authorLi, Huien_US
dc.contributor.authorLi, Shengtaien_US
dc.contributor.authorWeaver, Eriken_US
dc.contributor.authorBoehler, Yannen_US
dc.contributor.authorCarperter, John M.en_US
dc.contributor.authorDe Gregorio-Monsalvo, Itziaren_US
dc.contributor.authorManara, Carlo F.en_US
dc.contributor.authorNatta, Antonellaen_US
dc.contributor.authorPérez, Laura M.en_US
dc.contributor.authorRicci, Lucaen_US
dc.contributor.authorSargent, Anneilaen_US
dc.contributor.authorTazzari, Marcoen_US
dc.contributor.authorTurner, Nealen_US
dc.date.accessioned2017-01-30T17:29:31Z
dc.date.available2017-01-30T17:29:31Z
dc.date.issued2016en_US
dc.description.abstractWe present Atacama Large Millimeter and Submillimeter Array observations of the protoplanetary disk around the Herbig Ae star HD 163296 that trace the spatial distribution of millimeter-sized particles and cold molecular gas on spatial scales as small as 25 astronomical units (A.U.). The image of the disk recorded in the 1.3 mm continuum emission reveals three dark concentric rings that indicate the presence of dust depleted gaps at about 60, 100, and 160 A.U. from the central star. The maps of the 12CO, 13CO, and C18O J=2−1 emission do not show such structures but reveal a change in the slope of the radial intensity profile across the positions of the dark rings in the continuum image. By comparing the observations with theoretical models for the disk emission, we find that the density of CO molecules is reduced inside the middle and outer dust gaps. However, in the inner ring there is no evidence of CO depletion. From the measurements of the dust and gas densities, we deduce that the gas-to-dust ratio varies across the disk and, in particular, it increases by at least a factor 5 within the inner dust gap compared to adjacent regions of the disk. The depletion of both dust and gas suggests that the middle and outer rings could be due to the gravitational torque exerted by two Saturn-mass planets orbiting at 100 and 160 A.U. from the star. On the other hand, the inner dust gap could result from dust accumulation at the edge of a magnetorotational instability dead zone, or from dust opacity variations at the edge of the CO frost line. Observations of the dust emission at higher angular resolution and of molecules that probe dense gas are required to establish more precisely the origins of the dark rings observed in the HD 163296 disk.en_US
dc.identifier.citationIsella, Andrea, Guidi, Greta, Testi, Leonardo, et al.. "Ringed Structures of the HD 163296 Protoplanetary Disk Revealed by ALMA." <i>Physical Review Letters,</i> 114, no. 25 (2016) American Physical Society: http://dx.doi.org/10.1103/PhysRevLett.117.251101.
dc.identifier.doihttp://dx.doi.org/10.1103/PhysRevLett.117.251101en_US
dc.identifier.urihttps://hdl.handle.net/1911/93807
dc.language.isoengen_US
dc.publisherAmerican Physical Society
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
dc.titleRinged Structures of the HD 163296 Protoplanetary Disk Revealed by ALMAen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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