Dynamics of the fast solar tachocline

Details Dynamics of the fast solar tachocline Dynamics of the fast solar tachocline

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508...79f&link_type=abstract

In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze

Computer Science

Sun: Interior, Mhd, Tachocline

Scientific paper

One possible scenario for the origin of the solar tachocline, known as the "fast tachocline", assumes that the turbulent diffusivity exceeds η >= 109cm2/s. In this case the dynamics will be governed by the dynamo-generated oscillatory magnetic field on relatively short timescales. Here, for the first time, we present detailed numerical models for the fast solar tachocline with all components of the magnetic field calculated explicitly, assuming axial symmetry and a constant turbulent diffusivity η and viscosity ν. We find that a sufficiently strong oscillatory poloidal field with dipolar latitude dependence at the tachocline-convective zone boundary is able to confine the tachocline. The thickness of the tachocline shows a marked dependence on both time and latitude. We also examined the influence of the meridional flow (amplitude -3 to +3 cm/s) on the thickness of the tachocline.

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