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Invited speaker: Solar Tachocline Confinement by a Dynamo with Deep Extent

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DY2W03 - Modeling, observing and understanding flows and magnetic fields in the Earth's core and in the Sun

In the solar tachocline at the base of the convection zone, strong latitudinal differential rotation transitions to nearly solid-body rotation in the underlying radiative interior. The observed thinness of the tachocline remains largely unexplained, given that diffusive processes acting over the Sun’s main-sequence lifetime are expected to have imprinted the latitudinal differential rotation deep into the radiative interior. Here, we present a global MHD simulation in which a non-axisymmetric, cycling dynamo forces the radiative interior into solid-body rotation. The magnetic torque counters viscous tachocline spread by a process similar to Ferraro’s law of isorotation, as applied to a longitudinally and temporally varying magnetic field. Furthermore, there is dynamo-amplified field even below the convective overshoot layer, driven there by strong horizontal motions that are in part due to equatorially confined Rossby waves. We discuss this simulation in light of the proposed fast magnetic tachocline confinement scenario and the depth to which the solar dynamo extends.

This talk is part of the Isaac Newton Institute Seminar Series series.

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