Volume 483, Number 3, June I 2008
|Page(s)||949 - 960|
|Section||Numerical methods and codes|
|Published online||26 March 2008|
A solar mean field dynamo benchmark
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, DAPNIA/SAp, 91191 Gif sur Yvette, France e-mail: email@example.com
2 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
3 Nordita, AlbaNova University Center, Roslagstullsbacken 23, 10691 Stockholm, Sweden
4 High Altitude Observatory, National Center for Atmospheric Research, 3080 Center Green, Boulder, CO 80301, USA
5 INAF Osservatorio Astrofisico di Catania, via S.Sofia 78, 95123 Catania, Italy
6 Observatory, PO Box 14, 00014 University of Helsinki, Finland
7 School of Mathematics, University of Manchester, Manchester M13 9PL, UK
8 W.W. Hansen Experimental Physics Laboratory, Stanford University, USA
Accepted: 29 February 2008
Context. The solar magnetic activity and cycle are linked to an internal dynamo. Numerical simulations are an efficient and accurate tool to investigate such intricate dynamical processes.
Aims. We present the results of an international numerical benchmark study based on two-dimensional axisymmetric mean field solar dynamo models in spherical geometry. The purpose of this work is to provide reference cases that can be analyzed in detail and that can help in further development and validation of numerical codes that solve such kinematic problems.
Methods. The results of eight numerical codes solving the induction equation in the framework of mean field theory are compared for three increasingly computationally intensive models of the solar dynamo: an dynamo with constant magnetic diffusivity, an dynamo with magnetic diffusivity sharply varying with depth and an example of a flux-transport Babcock-Leighton dynamo which includes a non-local source term and one large single cell of meridional circulation per hemisphere. All cases include a realistic profile of differential rotation and thus a sharp tachocline.
Results. The most important finding of this study is that all codes agree quantitatively to within less than a percent for the dynamo cases and within a few percent for the flux-transport case. Both the critical dynamo numbers for the onset of dynamo action and the corresponding cycle periods are reasonably well recovered by all codes. Detailed comparisons of butterfly diagrams and specific cuts of both toroidal and poloidal fields at given latitude and radius confirm the good quantitative agreement.
Conclusions. We believe that such a benchmark study will be a very useful tool since it provides detailed standard cases for comparison and reference.
Key words: Sun: magnetic fields / Sun: activity / Sun: interior / methods: numerical
© ESO, 2008
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