  We aim at estimating the dust scale height of protoplanetary disks from
millimeter continuum observations. First, we present a general expression of
intensity of a ring in a protoplanetary disk, and show that we can constrain
the dust scale height by the azimuthal intensity variation. Then, we apply the
presented methodology to the two distinct rings at 68 au and at 100 au of the
protoplanetary disk around HD 163296. We constrain the dust scale height by
comparing the DSHARP high-resolution millimeter dust continuum image with
radiative transfer simulations using RADMC-3D. We find that h_d/h_g > 0.84 at
the inner ring and h_d/h_g < 0.11 at the outer ring with the 3 sigma
uncertainties, where h_d is the dust scale height and h_g is the gas scale
height. This indicates that the dust is flared at the inner ring and settled at
the outer ring. We further constrain the ratio of turbulence parameter alpha to
gas-to-dust-coupling parameter St from the derived dust scale height; alpha/St
> 2.4 at the inner ring, and alpha/St < 1.1*10^{-2} at the outer ring. This
result shows that the turbulence is stronger or the dust is smaller at the
inner ring than at the outer ring.
