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It has recently been recognized that the convective velocities achieved inthe current solar convection simulations might be over-estimated. Thenewly-revealed effects of the prevailing small-scale magnetic field within theconvection zone may offer possible solutions to this problem. The small-scalemagnetic fields can reduce the convective amplitude of small-scale motionsthrough the Lorentz-force feedback, which concurrently inhibits the turbulentmixing of entropy between upflows and downflows. As a result, the effectivePrandtl number may exceed unity inside the solar convection zone. In thispaper, we propose and numerically confirm a possible suppression mechanism ofconvective velocity in the effectively high-Prandtl number regime. If theeffective horizontal thermal diffusivity decreases (the Prandtl numberaccordingly increases), the subadiabatic layer which is formed near the base ofthe convection zone by continuous depositions of low entropy transported byadiabatically downflowing plumes is enhanced and extended. The globalconvective amplitude in the high-Prandtl thermal convection is thus reducedespecially in the lower part of the convection zone via the change in the meanentropy profile which becomes more subadiabatic near the base and lesssuperadiabatic in the bulk.

Convective velocity suppression via the enhancement of subadiabatic layer: Role of the effective Prandtl number