Vorticity Budget of Weak Thermal Convection in Keplerian disks

Abstract

By employing the equations of mean-square vorticity (enstrophy) fluctuations in strong shear flows, we demonstrate that unlike energy production of turbulent vorticity in nonrotating shear flows, the turbulent vorticity of weak convection in Keplerian disks cannot gain energy from vortex stretching/tilting by background shear unless the asscoiated Reynolds stresses are negative. This is because the epicyclic motion is an energy sink of the radial component of mean-square turbulent vorticity in Keplerian disks when Reynolds stresses are positive. Consequently, weak convection cannot be self-sustained in Keplerian flows. This agrees with the results implied from the equations of mean-square velocity fluctuations in strong shear flows. Our analysis also sheds light on the explanation of the simulation result in which positive kinetic helicity is produced by the Balbus-Hawley instability in a vertically stratified Keplerian disk. We also comment on the possibility of outward angular momentum transport by strong convection based on azimuthal pressure perturbations and directions of energy cascade.

8 pages, 1 figure, emulateapj.sty, revised version in response to referee's comments, accepted by ApJ

References in corpus (5)

• The Formation and Structure of a Strongly Magnetized Corona above Weakly Magnetized Accretion Disks
• Convection-Dominated Accretion Flows
• Self-Similar Accretion Flows with Convection
• Stability, Instability, and "Backwards'' Transport in Accretion Disks"
• Thermal Equilibrium Curves and Turbulent Mixing in Keplerian Accretion Disks