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Robustness of oscillatory α 2 dynamos in spherical wedges
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.ORCID iD: 0000-0002-7304-021X
2016 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 593, A134Article in journal (Refereed) Published
Abstract [en]

Context. Large-scale dynamo simulations are sometimes confined to spherical wedge geometries by imposing artificial boundary conditions at high latitudes. This may lead to spatio-temporal behaviours that are not representative of those in full spherical shells. Aims. We study the connection between spherical wedge and full spherical shell geometries using simple mean-field dynamos. Methods. We solve the equations for one-dimensional time-dependent α2 and α2Ω mean-field dynamos with only latitudinal extent to examine the effects of varying the polar angle θ0 between the latitudinal boundaries and the poles in spherical coordinates. Results. In the case of constant α and ηt profiles, we find oscillatory solutions only with the commonly used perfect conductor boundary condition in a wedge geometry, while for full spheres all boundary conditions produce stationary solutions, indicating that perfect conductor conditions lead to unphysical solutions in such a wedge setup. To search for configurations in which this problem can be alleviated we choose a profile of the turbulent magnetic diffusivity that decreases toward the poles, corresponding to high conductivity there. Oscillatory solutions are now achieved with models extending to the poles, but the magnetic field is strongly concentrated near the poles and the oscillation period is very long. By changing both the turbulent magnetic diffusivity and α profiles so that both effects are more concentrated toward the equator, we see oscillatory dynamos with equatorward drift, shorter cycles, and magnetic fields distributed over a wider range of latitudes. Those profiles thus remove the sensitive and unphysical dependence on θ0. When introducing radial shear, we again see oscillatory dynamos, and the direction of drift follows the Parker-Yoshimura rule. Conclusions. A reduced α effect near the poles with a turbulent diffusivity concentrated toward the equator yields oscillatory dynamos with equatorward migration and reproduces best the solutions in spherical wedges. For weak shear, oscillatory solutions are obtained only for perfect conductor field conditions and negative shear. Oscillatory solutions become preferred at sufficiently strong shear. Recent three-dimensional dynamo simulations producing solar-like magnetic activity are expected to lie in this range.

Place, publisher, year, edition, pages
2016. Vol. 593, A134
Keyword [en]
Hydrodynamics, Magnetohydrodynamics (MHD), Turbulence, Boundary conditions, Diffusion, Geometry, Interactive devices, Magnetic fields, Magnetism, Spheres, Artificial boundary condition, High conductivity, Magnetic diffusivity, Oscillation periods, Oscillatory solutions, Spherical coordinates, Stationary solutions, Turbulent diffusivities, Magnetohydrodynamics
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-194889DOI: 10.1051/0004-6361/201628165ISI: 000385820100045ScopusID: 2-s2.0-84990244245OAI: oai:DiVA.org:kth-194889DiVA: diva2:1053093
Note

QC 20161208

Available from: 2016-12-08 Created: 2016-11-01 Last updated: 2016-12-14Bibliographically approved

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Citation style
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