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The building of planetary systems is controlled by the gas and dust dynamicsof protoplanetary disks. While the gas is simultaneously accreted onto thecentral star and dissipated away by winds, dust grains aggregate and collapseto form planetesimals and eventually planets. This dust and gas dynamicsinvolves instabilities, turbulence and complex non-linear interactions whichultimately control the observational appearance and the secular evolution ofthese disks.  This chapter is dedicated to the most recent developments in ourunderstanding of the dynamics of gaseous and dusty disks, covering hydrodynamicand magnetohydrodynamic turbulence, gas-dust instabilities, dust clumping anddisk winds. We show how these physical processes have been tested fromobservations and highlight standing questions that should be addressed in thefuture.

Hydro-, Magnetohydro-, and Dust-Gas Dynamics of Protoplanetary Disks