Show simple item record

dc.contributor.authorMuro-Arena, G.A.
Dominik, C.
Waters, L.B.F.M.
Min, M.
Klarmann, L.
Ginski, C.
Isella, A.
Benisty, M.
Pohl, A.
Garufi, A.
Hagelberg, J.
Langlois, M.
Menard, F.
Pinte, C.
Sezestre, E.
van der Plas, G.
Villenave, M.
Delboulbé, A.
Magnard, Y.
Möller-Nilsson, O.
Pragt, J.
Rabou, P.
Roelfsema, R.
dc.date.accessioned 2018-09-26T14:52:40Z
dc.date.available 2018-09-26T14:52:40Z
dc.date.issued 2018
dc.identifier.citation Muro-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?." Astronomy & Astrophysics, 614, (2018) https://doi.org/10.1051/0004-6361/201732299.
dc.identifier.urihttps://hdl.handle.net/1911/102707
dc.description.abstract Context. 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.
dc.language.iso eng
dc.rights Article 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.title Dust modeling of the combined ALMA and SPHERE datasets of HD 163296. Is HD 163296 really a Meeus group II disk?
dc.type Journal article
dc.citation.journalTitle Astronomy & Astrophysics
dc.subject.keywordprotoplanetary disks
scattering
techniques: polarimetric
techniques: interferometric
stars: individual: HD 163296
dc.citation.volumeNumber 614
dc.identifier.digital aa32299-17
dc.contributor.publisher EDP Sciences
dc.type.dcmi Text
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201732299
dc.type.publication publisher version
dc.citation.articleNumber A24


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record