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A complete and detailed knowledge of the structure of the gaseous componentin protoplanetary discs is essential to the study of dust evolution during theearly phases of pre-planetesimal formation. The aim of this paper is todetermine if three-dimensional accretion discs simulated by the SmoothedParticle Hydrodynamics (SPH) method can reproduce the observational data nowavailable and the expected turbulent nature of protoplanetary discs. Theinvestigation is carried out by setting up a suite of diagnostic toolsspecifically designed to characterise both the global flow and the fluctuationsof the gaseous disc. The main result concerns the role of the artificialviscosity implementation in the SPH method: in addition to the already knownability of SPH artificial viscosity to mimic a physical-like viscosity underspecific conditions, we show how the same artificial viscosity prescriptionbehaves like an implicit turbulence model. In fact, we identify a threshold forthe parameters in the standard artificial viscosity above which SPH disc modelspresent a cascade in the power spectrum of velocity fluctuations, turbulentdiffusion and a mass accretion rate of the same order of magnitude as measuredin observations. Furthermore, the turbulence properties observed locally in SPHdisc models are accompanied by meridional circulation in the global flow of thegas, proving that the two mechanisms can coexist.

Characterisation of global flow and local fluctuations in 3D SPH simulations of protoplanetary discs