Turbulence is playing a key role in planet forming disks. It modifies the dust drift toward the star, the grains relative velocity and therefore their possible growth, turbulence can also form dust clump that may gravitationally collapse and transport angular momentum through the disk. Understanding the properties of the turbulent state in protoplanetary disk is therefore a major effort for the understanding of planet formation. However the complex physical context of planet formation render the study of turbulence in these disks highly non trivial. The Keplerian shear tend to remove energy from the turbulent state, whereas rotation is known to ellongate vertically the turbulent eddies. We have already studied particle dynamics in incompressible keplerian turbulence and identified new mecanisms participating to planetesimal formation. The aim of this intership is to provide a first caracterisation of the properties of turbulence in a Keplerain flow when a weak compressibility is considered. The student will run and analyse the results of numerical simulations of forced turbulence in a Keplerian flow. The student will developp a physical understanding of process involved in the turbulent cascade of such astrophysical flows.