Stability of the solar tachocline with magnetic fields

Details Stability of the solar tachocline with magnetic fields Stability of the solar tachocline with magnetic fields

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007an....328.1142a&link_type=abstract

Astronomische Nachrichten, Vol.328, Issue 10, p.1142

Astronomy and Astrophysics

Astronomy

3

Sun: Magnetic Fields, Instabilities

Scientific paper

The stability of magnetic fields in the solar tachocline is investigated. We present stability limits for higher azimuthal wave numbers and results on the dependence of the stability on the location of toroidal magnetic fields in latitude. While the dependence of the wave number with the largest growth rate on the magnetic field strength and the magnetic Prandtl number is small, the dependence on the magnetic Reynolds number Rm indicates that lowest azimuthal modes are excited for very high Rm. Upon varying the latitudinal position of the magnetic field belts, we find slightly lower stability limits for high latitudes, and very large stability limits at latitudes below 10o, with little dependence on latitude in between. An increase of the maximum possible field was achieved by adding a poloidal field. The upper limit for the toroidal field which can be stored in the radiative tachocline is then 1000 G, compared to about 100 G for a purely toroidal field as was found in an earlier work.

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