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This paper deals with the problem of hydrodynamic shear turbulence innon-magnetized Keplerian disks. We wish to draw attention to a route tohydrodynamic turbulence which seems to be little known by the astrophysicalcommunity, but which has been intensively discussed among fluid dynamicistsduring the past decade. In this so-called `bypass' concept for the onset ofturbulence, perturbations undergo a transient growth, and they may reach anamplitude that is sufficiently large to allow positive feedback throughnonlinear interactions. This transient growth is linear in nature, and thus itdiffers in principle from the well-known nonlinear instability. We describe thetype of perturbations that according to this process are the most likely tolead to turbulence, namely non-axisymmetric vortex mode perturbations in thetwo dimensional limit. We show that the apparently inhibiting action of theCoriolis force on the dynamics of such vortical perturbations is substantiallydiminished due to the pressure perturbations, contrary to current opinion. Westress the similarity of the turbulent processes in Keplerian disks and inCartesian flows and conclude that the prevalent skepticism of the astrophysicalcommunity on the occurrence of hydrodynamic shear turbulence in such disks isnot founded.Comment: 8 pages, 1 figure, accepted in A &

On hydrodynamic shear turbulence in Keplerian disks: Via transient growth to bypass transition