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The influence of stratification upon small-scale convectively-driven dynamos

Published online by Cambridge University Press:  12 August 2011

Paul J. Bushby ,
Michael R. E. Proctor  and
Nigel O. Weiss
Paul J. Bushby
Affiliation:
School of Mathematics and Statistics, Newcastle University, Newcastle upon Tyne, NE1 7RU, U.K. email: paul.bushby@ncl.ac.uk
Michael R. E. Proctor
Affiliation:
Department of Applied Mathematics and Theoretical Physics (DAMTP), University of Cambridge, Cambridge CB3 0WA, U.K. email: mrep@cam.ac.uk (MREP) and now@cam.ac.uk (NOW)
Nigel O. Weiss
Affiliation:
Department of Applied Mathematics and Theoretical Physics (DAMTP), University of Cambridge, Cambridge CB3 0WA, U.K. email: mrep@cam.ac.uk (MREP) and now@cam.ac.uk (NOW)
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Abstract

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In the quiet Sun, convective motions form a characteristic granular pattern, with broad upflows enclosed by a network of narrow downflows. Magnetic fields tend to accumulate in the intergranular lanes, forming localised flux concentrations. One of the most plausible explanations for the appearance of these quiet Sun magnetic features is that they are generated and maintained by dynamo action resulting from the local convective motions at the surface of the Sun. Motivated by this idea, we describe high resolution numerical simulations of nonlinear dynamo action in a (fully) compressible, non-rotating layer of electrically-conducting fluid. The dynamo properties depend crucially upon various aspects of the fluid. For example, the magnetic Reynolds number (Rm) determines the initial growth rate of the magnetic energy, as well as the final saturation level of the dynamo in the nonlinear regime. We focus particularly upon the ways in which the Rm-dependence of the dynamo is influenced by the level of stratification within the domain. Our results can be related, in a qualitative sense, to solar observations.

Keywords

Convectionmagnetic fields(magnetohydrodynamics:) MHDSun: magnetic fieldsSun: photosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 197 - 204
Copyright
Copyright © International Astronomical Union 2011

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