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 spatially resolved in millimeter-wave polarization measurements .
In this paper , we conduct radiative transfer modeling that includes self-scattering polarization to constrain the grain size and its distribution .
We found that the grain size and dust scale height are the key parameters for reproducing the radial and azimuthal distributions of the observed polarization signature .
Radial variation is mainly determined by grain size .
The polarization fraction is high if the particle size is \sim \lambda / 2 \pi ; it is low if the particle size is larger or smaller than this .
In contrast , azimuthal variation in polarization is enhanced if the dust scale height is increased .
Based on detailed modeling of the HD 163296 polarization , we found the following radial variations in the grain size and dust scale height .
The maximum grain size was 140 microns in the gaps and significantly larger or smaller in the rings .
The dust scale height is less than one-third the gas scale height inside the 70 au ring , and two-thirds the gas scale height outside the 70 au ring .
Furthermore , we constrained the gas turbulence to be \alpha \lesssim 1.5 \times 10 ^ { -3 } in the 50 au gap and \alpha \sim 0.015 - 0.3 in the 90 au gap .
The transition of the turbulence strength at the boundary of the 70 au ring indicates the existence of a dead zone .