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This review examines recent theoretical developments in our understanding ofturbulence in cold, non-magnetically active, planetesimal forming regions ofprotoplanetary disks which we refer to throughout as "Ohmic zones". We give abrief background introduction to the subject of disk turbulence followed by aterse pedagogical review of the phenomenology of hydrodynamic turbulence. Theequations governing the dynamics of cold astrophysical disks are given andbasic flow states are described. We discuss the Solberg-Hoiland conditionsrequired for stability, and the three recently identified turbulence generatingmechanisms possibly active in protoplanetary disk Ohmic zones, namely, (i) theVertical Shear Instability, (ii) The Convective Overstability and (iii) theZombie Vortex Instability. We summarize the properties of these processes,identify their limitations and discuss where and under what conditions theseprocesses are active in protoplanetary disk Ohmic zones.

The initial conditions for planet formation: Turbulence driven by hydrodynamical instabilities in disks around young stars