Formation of buoyant magnetic structures by a localized velocity shear

Details Formation of buoyant magnetic structures by a localized velocity shear Formation of buoyant magnetic structures by a localized velocity shear

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.329l..73b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 329, Issue 4, pp. L73-L76.

Astronomy and Astrophysics

Astronomy

24

Mhd, Sun: Interior, Sun: Magnetic Fields, Stars: Spots

Scientific paper

Motivated by considerations of the solar tachocline, we study the generation of strong buoyant magnetic structures by a sheared velocity field localized in a convectively stable background, using non-linear three-dimensional (3D) magnetohydrodynamic (MHD) simulations. The shear flow can spontaneously create strong tube-like toroidal (streamwise) magnetic structures from an imposed weak uniform poloidal (cross-stream) magnetic field. The structures are magnetically buoyant and therefore rise, and may evolve further to a rich variety of geometries, including kinked or arched shapes. The emergence process can repeat indefinitely with a characteristic period. These mechanisms may be relevant to the MHD processes in the solar tachocline and the creation and emergence of solar active regions.

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