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Recent Atacama Large Millimeter and Submillimeter Array (ALMA) observationsof the protoplanetary disk around the Herbig Ae star HD 163296 revealed threedepleted dust gaps at 60, 100 and 160 au in the 1.3 mm continuum as well as COdepletion in the middle and outer dust gaps. However, no CO depletion was foundin the inner dust gap. To examine the planet--disk interaction model, wepresent results of two-dimensional two fluid (gas + dust) hydrodynamicsimulations coupled with three-dimensional radiative transfer simulations. Inorder to fit the high gas-to-dust ratio of the first gap, we find theShakura--Sunyaev viscosity parameter $\alpha$ must be very small ($\lesssim10^{-4}$) in the inner disk. On the other hand, a relatively large $\alpha$($\sim 7.5\times 10^{-3}$) is required to reproduce the dust surface density inthe outer disk. We interpret the variation of $\alpha$ as an indicator of thetransition from an inner dead zone to the outer magnetorotational instability(MRI) active zone. Within $\sim 100$ au, the HD 163296 disk's ionization levelis low, and non-ideal magnetohydrodynamic (MHD) effects could suppress the MRI,so the disk can be largely laminar. The disk's ionization level graduallyincreases toward larger radii, and the outermost disk ($r > 300$ au) becomesturbulent due to MRI. Under this condition, we find that the observed dustcontinuum and CO gas line emissions can be reasonably fit by threehalf-Jovian-mass planets (0.46, 0.46 and 0.58 $M_\textrm{J}$) at 59, 105 and160 au, respectively.

New constraints on turbulence and embedded planet mass in the HD 163296 disk from planet-disk hydrodynamic simulations