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

Muro-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.

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Journal Article

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

MPS-Authors

Muro-Arena, G. A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dominik, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Waters, L. B. F. M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Min, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Klarmann, L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ginski, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Isella, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Benisty, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pohl, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Garufi, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hagelberg, J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Langlois, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Menard, F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pinte, C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sezestre, E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van der Plas, G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Villenave, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Delboulbé, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Magnard, Y.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Möller-Nilsson, O.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pragt, J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rabou, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Roelfsema, R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018A&A...614A..24M
(Any fulltext)

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Muro-Arena, G. A., Dominik, C., Waters, L. B. F. M., Min, M., Klarmann, L., Ginski, C., et al. (2018). Dust modeling of the combined ALMA and SPHERE datasets of HD 163296. Is HD 163296 really a Meeus group II disk? Astronomy and Astrophysics, 614.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CC08-D

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.