Volume 453, Number 2, July II 2006
|Page(s)||687 - 698|
|Section||Stellar structure and evolution|
|Published online||16 June 2006|
The stability of toroidal fields in stars
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, Postfach 1317, 85741 Garching, Germany e-mail: firstname.lastname@example.org
Accepted: 21 March 2006
We present numerical models of hydromagnetic instabilities under the conditions prevailing in a stably stratified, non-convective stellar interior, and compare them with previous results of analytic work on instabilities in purely toroidal fields. We confirm that an mode (“kink”) is the dominant instability in a toroidal field in which the field strength is proportional to distance from the axis, such as the field formed by the winding up of a weak field by differential rotation. We measure the growth rate of the instability as a function of field strength and rotation rate Ω, and investigate the effects of a stabilising thermal stratification as well as magnetic and thermal diffusion on the stability. Where comparison is computationally feasible, the results agree with analytic predictions.
Key words: instabilities / magnetohydrodynamics (MHD) / stars: magnetic fields
© ESO, 2006
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