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SUMMARY:The Rotational Influence on Solar Convection - Keith Julien (Unive
 rsity of Colorado Boulder)
DTSTART:20220519T150000Z
DTEND:20220519T160000Z
UID:TALK173585@talks.cam.ac.uk
DESCRIPTION:The observational absence of giant convection cells near the S
 un&rsquo\;s outer surface is a long- standing conundrum for solar modelers
 . We herein propose an explanation. Rotation strongly influences the inter
 nal dynamics\, leading to suppressed convective velocities\, enhanced ther
 mal-transport efficiency\, and (most significantly) relatively smaller dom
 inant length scales. We specifically predict a characteristic convection l
 ength scale of roughly 30 Mm throughout much of the convection zone\, impl
 ying weak ow amplitudes at 100- 200 Mm giant cells scales\, representative
  of the total envelope depth. Our reasoning is such that: Coriolis forces 
 primarily balance pressure gradients (geostrophy). Background vortex stret
 ching balances baroclinic torques. Both together balance nonlinear advecti
 on. Turbulent fluxes convey the excess part of the solar luminosity that r
 adiative diffusion cannot. We show that these four relations determine est
 imates for the dominant length scales and dynamical amplitudes strictly in
  terms of known physical quantities. We predict that the dynamical Rossby 
 number for convection is less than unity below the near-surface shear laye
 r\, indicating rotational constraint.
LOCATION:Seminar Room 1\, Newton Institute
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