Confinement of Magnetic Fields Below the Solar Convection Zone
Confining the primordial dipole magnetic field below the convection zone affords the possibility of a serendipitous solution that fits many of the observed qualities of the solar interior rotation profile. Gough and McIntyre [<xref ref-type="bibr" rid="CR6">6</xref>] pointed this out and derived a laminar balanced model that operates on the slow Eddington-Sweet timescale for this purpose. An interesting question is, what is the role of turbulence? Does the presence of turbulence help or hinder? In the spirit of Michael Thompson's love of tachocline dynamics, we survey some recent work on these issues.
Dynamics of the Sun and Stars; Honoring the Life and Work of Michael J. Thompson
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