Deep magnetic field stretching in numerical dynamos

Abstract The process of magnetic field stretching transfers kinetic energy to magnetic energy and thereby maintains dynamos against ohmic dissipation. Stretching at depth may play an important role in shaping the field morphology and in the dynamo action. Here, we analyze snapshots from self-consist...

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Main Authors: Diego Peña, Hagay Amit, Katia J. Pinheiro
Format: Article
Language:English
Published: SpringerOpen 2018-02-01
Series:Progress in Earth and Planetary Science
Subjects:
Online Access:http://link.springer.com/article/10.1186/s40645-017-0162-5
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spelling doaj-33924b9d187844c09aaa42901cf8599b2020-11-24T21:51:53ZengSpringerOpenProgress in Earth and Planetary Science2197-42842018-02-015112310.1186/s40645-017-0162-5Deep magnetic field stretching in numerical dynamosDiego Peña0Hagay Amit1Katia J. Pinheiro2Geophysics Department, Observatório NacionalCNRS, Université de Nantes, Nantes Atlantiques Universités, UMR CNRS 6112, Laboratoire de Planétologie et de GéodynamiqueGeophysics Department, Observatório NacionalAbstract The process of magnetic field stretching transfers kinetic energy to magnetic energy and thereby maintains dynamos against ohmic dissipation. Stretching at depth may play an important role in shaping the field morphology and in the dynamo action. Here, we analyze snapshots from self-consistent 3D numerical dynamos to unravel the nature of field-flow interactions that induces stretching secular variation of the radial magnetic field at mid-depth of the shell. We search for roots of intense flux patches identified at the outer boundary. The deep radial field structures exhibit a position shift with respect to the locations of the outer boundary patches, consistent with a mixed effect of tangent cylinder rim and plume-like dynamics. A global stretching/advection rms ratio is ∼ 1.5–3 times larger than that of poloidal/toroidal flows. In addition, local stretching is often more effective than advection, in particular at regions of significant field-aligned flow. On average at roots of high-latitude flux patches, total stretching is 1.1 times larger than total advection despite the poloidal flow being only 0.37 of the toroidal flow. Radial stretching secular variation acts as an effective dynamo mechanism at regions where laterally varying radial flow shears toroidal field lines to generate a poloidal magnetic field. Stretching at depth exhibits similar parameter dependence as that of stretching at the outer boundary, with the strongest dependence being on the magnetic Prandtl number in both cases. Our results provide insights into the underlying deep dynamo mechanisms that sustain intense magnetic flux patches at the outer boundary.http://link.springer.com/article/10.1186/s40645-017-0162-5Magnetic fieldDynamoStretchingFlux patchSecular variationCore stratification
collection DOAJ
language English
format Article
sources DOAJ
author Diego Peña
Hagay Amit
Katia J. Pinheiro
spellingShingle Diego Peña
Hagay Amit
Katia J. Pinheiro
Deep magnetic field stretching in numerical dynamos
Progress in Earth and Planetary Science
Magnetic field
Dynamo
Stretching
Flux patch
Secular variation
Core stratification
author_facet Diego Peña
Hagay Amit
Katia J. Pinheiro
author_sort Diego Peña
title Deep magnetic field stretching in numerical dynamos
title_short Deep magnetic field stretching in numerical dynamos
title_full Deep magnetic field stretching in numerical dynamos
title_fullStr Deep magnetic field stretching in numerical dynamos
title_full_unstemmed Deep magnetic field stretching in numerical dynamos
title_sort deep magnetic field stretching in numerical dynamos
publisher SpringerOpen
series Progress in Earth and Planetary Science
issn 2197-4284
publishDate 2018-02-01
description Abstract The process of magnetic field stretching transfers kinetic energy to magnetic energy and thereby maintains dynamos against ohmic dissipation. Stretching at depth may play an important role in shaping the field morphology and in the dynamo action. Here, we analyze snapshots from self-consistent 3D numerical dynamos to unravel the nature of field-flow interactions that induces stretching secular variation of the radial magnetic field at mid-depth of the shell. We search for roots of intense flux patches identified at the outer boundary. The deep radial field structures exhibit a position shift with respect to the locations of the outer boundary patches, consistent with a mixed effect of tangent cylinder rim and plume-like dynamics. A global stretching/advection rms ratio is ∼ 1.5–3 times larger than that of poloidal/toroidal flows. In addition, local stretching is often more effective than advection, in particular at regions of significant field-aligned flow. On average at roots of high-latitude flux patches, total stretching is 1.1 times larger than total advection despite the poloidal flow being only 0.37 of the toroidal flow. Radial stretching secular variation acts as an effective dynamo mechanism at regions where laterally varying radial flow shears toroidal field lines to generate a poloidal magnetic field. Stretching at depth exhibits similar parameter dependence as that of stretching at the outer boundary, with the strongest dependence being on the magnetic Prandtl number in both cases. Our results provide insights into the underlying deep dynamo mechanisms that sustain intense magnetic flux patches at the outer boundary.
topic Magnetic field
Dynamo
Stretching
Flux patch
Secular variation
Core stratification
url http://link.springer.com/article/10.1186/s40645-017-0162-5
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