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On MHD rotational transport, instabilities and dynamo action in stellar radiation zones

  • Stéphane Mathis (a1) (a2), A.-S. Brun (a1) (a2) and J.-P. Zahn (a2)

Abstract

Magnetic field and their related dynamical effects are thought to be important in stellar radiation zones. For instance, it has been suggested that a dynamo, sustained by a m = 1 MHD instability of toroidal magnetic fields (discovered by Tayler in 1973), could lead to a strong transport of angular momentum and of chemicals in such stable regions. We wish here to recall the different magnetic transport processes present in radiative zone and show how the dynamo can operate by recalling the conditions required to close the dynamo loop (BPol → BTor → BPol). Helped by high-resolution 3D MHD simulations using the ASH code in the solar case, we confirm the existence of the m = 1 instability, study its non-linear saturation, but we do not detect, up to a magnetic Reylnods number of 105, any dynamo action.

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References

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Braithwaite, J. 2006, A&A 449, 451
Brun, A.-S. & Zahn, J.-P. 2006, A&A 457, 665
Brun, A.-S., Miesch, M. S. & Toomre, J. 2004, ApJ 614, 1073
Clune, T. L. et al. 1999, Parallel Comput. 25, 361
Gellert, M., Rüdiger, G., & Elstner, D. 2008, A&A 479, L33
Pitts, E. & Tayler, R. J. 1985, MNRAS 216, 139
Spruit, H. C. 2002, A&A 381, 923
Zahn, J.-P., Brun, A.-S., & Mathis, S. 2007, A&A 474, 145
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Keywords

On MHD rotational transport, instabilities and dynamo action in stellar radiation zones

  • Stéphane Mathis (a1) (a2), A.-S. Brun (a1) (a2) and J.-P. Zahn (a2)

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