From convective to stellar dynamos

Details From convective to stellar dynamos From convective to stellar dynamos

2011-03-28

arxiv.org/abs/1103.5475v1

Astrophysical Dynamics: From Stars to Galaxies, ed. IAU Symp. 271, N. Brummell, A.S. Brun, M.S. Miesch, & Y. Ponty, pp. 279-28

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

9 pages, 5 figures, to appear in IAU Symposium 271, proceedings (N. Brummell, A. S. Brun, M. S. Miesch, and Y. Ponty, eds.)

Scientific paper

10.1017/S1743921311017704

Convectively driven dynamos with rotation generating magnetic fields on scales large compared with the scale of the turbulent eddies are being reviewed. It is argued that such fields can be understood as the result of an alpha effect. Simulations in Cartesian domains show that such large-scale magnetic fields saturate on a time scale compatible with the resistive one, suggesting that the magnitude of the alpha effect is here still constrained by approximate magnetic helicity conservation. It is argued that, in the absence of shear and/or any other known large-scale dynamo effects, these simulations prove the existence of turbulent alpha^2-type dynamos. Finally, recent results are discussed in the context of solar and stellar dynamos.

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