Stability of toroidal magnetic fields in the solar tachocline

Details Stability of toroidal magnetic fields in the solar tachocline Stability of toroidal magnetic fields in the solar tachocline

Jan 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...461..295a&link_type=abstract

Astronomy and Astrophysics, Volume 461, Issue 1, January I 2007, pp.295-301

Astronomy and Astrophysics

Astrophysics

20

Sun: Magnetic Fields, Instabilities, Sun: Rotation, Magnetic Fields, Magnetohydrodynamics (Mhd)

Scientific paper

The stability of toroidal magnetic fields in the radiative interior of the Sun is studied in a three-dimensional environment. The underlying differential rotation in the tachocline depends on both latitude and radius. We found stability limits for toroidal fields of only 100 G even in the simplified, incompressible, but stably stratified case. Nonaxisymmetric modes are linearly unstable with a weak influence on the amplitude of the underlying differential rotation. We conclude that the tachocline is not a suitable location for the storage of magnetic fields as strong as 100 kG. Since the results are based on an extrapolation of the numerical computations to lower solar diffusivities, high-resolution calculations at higher magnetic Reynolds numbers are required.

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