2006/02/23 by Peter Todd Williams, Peter T. Williams, Williams, Peter Todd
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Fluid Dynamics and Turbulent Flows #Geophysics and Gravity Measurements #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0602502
Six pages, no figures, in Solar MHD: Theory and Observations, eds: J. W. Leibacher, H. Uitenbroek, & R. F. Stein, Astron. Soc. Pac. Conf. Ser
arxiv created 2006/02/23 · openalex publication_date 2006/02/23 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Previous work on the angular momentum balance and meridional circulation of the solar convective zone (SCZ) generally consists either of semi-analytic approaches in which a simple turbulence model is adopted, or full direct numerical simulation (DNS) of the hydrodynamics or magnetohydrodynamics (MHD). In both instances the inclusion of magnetic fields has been troublesome. Also, both approaches have had difficulty reproducing the known angular velocity profile of the SCZ; this is the Taylor Number Puzzle. I discuss preliminary work in which I incorporate magnetic fields into a viscoelastic turbulence model for the SCZ and apply this to the problem of meridional circulation and angular momentum balance. I suggest that such an approach may help solve the Taylor Number Puzzle of the SCZ and bring theoretical predictions for the large-scale motion of the SCZ in line with observations.