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The HD 163296 disk shows ring and gap substructures with ALMA observations.In addition, this is the only disk where the rings and gaps are spatiallyresolved in millimeter-wave polarization measurements. In this paper, weconduct radiative transfer modeling that includes self-scattering polarizationto constrain the grain size and its distribution. We found that the grain sizeand dust scale height are the key parameters for reproducing the radial andazimuthal distributions of the observed polarization signature. Radialvariation is mainly determined by grain size. The polarization fraction is highif the particle size is $\sim \lambda/2\pi$; it is low if the particle size islarger or smaller than this. In contrast, azimuthal variation in polarizationis enhanced if the dust scale height is increased. Based on detailed modelingof the HD 163296 polarization, we found the following radial variations in thegrain size and dust scale height. The maximum grain size was 140 microns in thegaps and significantly larger or smaller in the rings. The dust scale height isless than one-third the gas scale height inside the 70 au ring, and two-thirdsthe gas scale height outside the 70 au ring. Furthermore, we constrained thegas turbulence to be $\alpha\lesssim1.5\times10^{-3}$ in the 50 au gap and$\alpha\sim 0.015-0.3$ in the 90 au gap. The transition of the turbulencestrength at the boundary of the 70 au ring indicates the existence of a deadzone.

Radial variations in grain sizes and dust scale heights in the protoplanetary disk around HD 163296 revealed by ALMA polarization observation