Dust modeling of the combined ALMA and SPHERE datasets of HD 163296. Is HD 163296 really a Meeus group II disk?

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dc.citation.articleNumberA24en_US
dc.citation.journalTitleAstronomy & Astrophysicsen_US
dc.citation.volumeNumber614en_US
dc.contributor.authorMuro-Arena, G.A.en_US
dc.contributor.authorDominik, C.en_US
dc.contributor.authorWaters, L.B.F.M.en_US
dc.contributor.authorMin, M.en_US
dc.contributor.authorKlarmann, L.en_US
dc.contributor.authorGinski, C.en_US
dc.contributor.authorIsella, A.en_US
dc.contributor.authorBenisty, M.en_US
dc.contributor.authorPohl, A.en_US
dc.contributor.authorGarufi, A.en_US
dc.contributor.authorHagelberg, J.en_US
dc.contributor.authorLanglois, M.en_US
dc.contributor.authorMenard, F.en_US
dc.contributor.authorPinte, C.en_US
dc.contributor.authorSezestre, E.en_US
dc.contributor.authorvan der Plas, G.en_US
dc.contributor.authorVillenave, M.en_US
dc.contributor.authorDelboulbé, A.en_US
dc.contributor.authorMagnard, Y.en_US
dc.contributor.authorMöller-Nilsson, O.en_US
dc.contributor.authorPragt, J.en_US
dc.contributor.authorRabou, P.en_US
dc.contributor.authorRoelfsema, R.en_US
dc.date.accessioned2018-09-26T14:52:40Zen_US
dc.date.available2018-09-26T14:52:40Zen_US
dc.date.issued2018en_US
dc.description.abstractContext. Multiwavelength observations are indispensable in studying disk geometry and dust evolution processes in protoplanetary disks. Aims. We aim to construct a three-dimensional model of HD 163296 that is capable of reproducing simultaneously new observations of the disk surface in scattered light with the SPHERE instrument and thermal emission continuum observations of the disk midplane with ALMA. We want to determine why the spectral energy distribution of HD 163296 is intermediary between the otherwise well-separated group I and group II Herbig stars. Methods. The disk was modeled using the Monte Carlo radiative transfer code MCMax3D. The radial dust surface density profile was modeled after the ALMA observations, while the polarized scattered light observations were used to constrain the inclination of the inner disk component and turbulence and grain growth in the outer disk. Results. While three rings are observed in the disk midplane in millimeter thermal emission at ~80, 124, and 200 AU, only the innermost of these is observed in polarized scattered light, indicating a lack of small dust grains on the surface of the outer disk. We provide two models that are capable of explaining this difference. The first model uses increased settling in the outer disk as a mechanism to bring the small dust grains on the surface of the disk closer to the midplane and into the shadow cast by the first ring. The second model uses depletion of the smallest dust grains in the outer disk as a mechanism for decreasing the optical depth at optical and near-infrared wavelengths. In the region outside the fragmentation-dominated regime, such depletion is expected from state-of-the-art dust evolution models. We studied the effect of creating an artificial inner cavity in our models, and conclude that HD 163296 might be a precursor to typical group I sources.en_US
dc.identifier.citationMuro-Arena, G.A., Dominik, C., Waters, L.B.F.M., et al.. "Dust modeling of the combined ALMA and SPHERE datasets of HD 163296. Is HD 163296 really a Meeus group II disk?." <i>Astronomy & Astrophysics,</i> 614, (2018) EDP Sciences: https://doi.org/10.1051/0004-6361/201732299.en_US
dc.identifier.digitalaa32299-17en_US
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201732299en_US
dc.identifier.urihttps://hdl.handle.net/1911/102707en_US
dc.language.isoengen_US
dc.publisherEDP Sciencesen_US
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.en_US
dc.subject.keywordprotoplanetary disksen_US
dc.subject.keywordscatteringen_US
dc.subject.keywordtechniques: polarimetricen_US
dc.subject.keywordtechniques: interferometricen_US
dc.subject.keywordstars: individual: HD 163296en_US
dc.titleDust modeling of the combined ALMA and SPHERE datasets of HD 163296. Is HD 163296 really a Meeus group II disk?en_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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