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Poster communications

Topology and field strength in spherical, anelastic dynamo simulations

Abstract : Dynamo action, i.e. the self-amplification of a magnetic field by the flow of an electrically conducting fluid, is considered to be the main mechanism for the generation of magnetic fields of stars and planets. Intensive and systematic parameter studies by direct numerical simulations using the Boussinesq approximation revealed fundamental properties of these models. However, this approximation considers an incompressible conducting fluid, and is therefore not adequate to describe convection in highly stratified systems like stars or gas giants. A common approach to overcome this difficulty is then to use the anelastic approximation, that allows for a reference density profile while filtering out sound waves for a faster numerical integration. We present the results of a systematic parameter study of spherical anelastic dynamo models, and compare them with previous results obtained in the Boussinesq approximation. We discuss the influence of the stratification on the field geometry and the field strength, and also compare the different scaling laws for the velocity amplitude, the magnetic dissipation time, and the convective heat flux.
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Contributor : Raphaël Raynaud <>
Submitted on : Monday, January 6, 2020 - 4:24:54 AM
Last modification on : Tuesday, July 21, 2020 - 3:31:42 AM
Document(s) archivé(s) le : Tuesday, April 7, 2020 - 5:04:04 PM


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  • HAL Id : hal-02428473, version 1


Raphaël Raynaud, Martin Schrinner, Ludovic Petitdemange, Emmanuel Dormy. Topology and field strength in spherical, anelastic dynamo simulations. AGU Fall Meeting, Dec 2014, San Francisco, United States. ⟨hal-02428473⟩



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