Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sf2a.conf..561z&link_type=abstract
SF2A-2007: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics held in Grenoble, France, July
Astronomy and Astrophysics
Astrophysics
Scientific paper
We examine the MHD instabilities arising in the radiation zone of a differentially rotating star, in which a poloidal field of fossil origin is sheared into a toroidal field. The numerical solutions built with the 3-dimensional ASH code are compared with the predictions drawn from an analytical study of the Pitts & Tayler instability. This instability is manifestly present in our simulations, with its conspicuous m=1 dependence in azimuth. However, although the instability generated field reaches an energy comparable to that of the mean poloidal field, that field seems unaffected by the instability: it undergoes Ohmic decline, and is neither eroded nor regenerated by the instability. The instability is sustained as long as the differential rotation acting on the poloidal field is able to generate a toroidal field of sufficient strength but, up to a magnetic Reynolds number of 10^5, we observe no sign of dynamo action, of either mean field or fluctuation type, contrary to what was suggested by Spruit.
Brun Allan Sacha
Mathis Stephane
Zahn Jean-Paul
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