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The origin of hydrodynamic turbulence in rotating shear flow is a longstanding puzzle. Resolving it is especially important in astrophysics when theflow angular momentum profile is Keplerian which forms an accretion disk havingnegligible molecular viscosity. Hence, any viscosity in such systems must bedue to turbulence, arguably governed by magnetorotational instabilityespecially when temperature T >~ 10^5. However, such disks around quiescentcataclysmic variables, protoplanetary and star-forming disks, the outer regionsof disks in active galactic nuclei are practically neutral in charge because oftheir low temperature, and thus expected not to be coupled with the magneticfield appropriately to generate any transport due to the magnetorotationalinstability. This flow is similar to plane Couette flow including the Coriolisforce, at least locally. What drives their turbulence and then transport, whensuch flows do not exhibit any unstable mode under linear hydrodynamicperturbation? We demonstrate that the threedimensional secondary disturbance tothe primarily perturbed flow triggering elliptical instability may generatesignificant turbulent viscosity ranging 0.0001 <~ \nu_t <~ 0.1 to explaintransport in accretion flows.

Possible origin of viscosity in the Keplerian accretion disks due to secondary perturbation: Turbulent transport without magnetic field