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Context. Multi-wavelength observations are indispensable in studying diskgeometry and dust evolution processes in protoplanetary disks. Aims. We aimedto construct a 3-dimensional model of HD 163296 capable of reproducingsimultaneously new observations of the disk surface in scattered light with theSPHERE instrument and thermal emission continuum observations of the diskmidplane with ALMA. We want to determine why the SED of HD 163296 isintermediary between the otherwise well-separated group I and group II Herbigstars. Methods. The disk was modelled using the Monte Carlo radiative transfercode MCMax3D. The radial dust surface density profile was modelled after theALMA observations, while the polarized scattered light observations were usedto constrain the inclination of the inner disk component and turbulence andgrain growth in the outer disk. Results. While three rings are observed in thedisk midplane in millimeter thermal emission at $\sim$80, 124 and 200 AU, onlythe innermost of these is observed in polarized scattered light, indicating alack of small dust grains on the surface of the outer disk. We provide twomodels capable of explaining this difference. The first model uses increasedsettling in the outer disk as a mechanism to bring the small dust grains on thesurface of the disk closer to the midplane, and into the shadow cast by thefirst ring. The second model uses depletion of the smallest dust grains in theouter disk as a mechanism for decreasing the optical depth at optical and NIRwavelengths. In the region outside the fragmentation-dominated regime, suchdepletion is expected from state-of-the-art dust evolution models. We studiedthe effect of creating an artificial inner cavity in our models, and concludethat HD 163296 might be a precursor to typical group I sources.

Dust modeling of the combined ALMA and SPHERE datasets of HD163296. Is HD163296 really a Meeus group II disk?