Large-scale model of the axisymmetric kinematic dynamo
A formulation of a kinematic dynamo is presented, based on a previously derived self-consistent procedure for obtaining large-scale models for complex system of equations. The model has only a small number of parametrized variables: the small-scale magnetic diffusivity, the scale of the large-scale...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2016 |
| País: | Argentina |
| Institución: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositorio: | CONICET Digital (CONICET) |
| Idioma: | inglés |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/182440 |
| Acceso en línea: | http://hdl.handle.net/11336/182440 |
| Access Level: | acceso abierto |
| Palabra clave: | DYNAMO MAGNETIC FIELDS MHD TURBULENCE https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Sumario: | A formulation of a kinematic dynamo is presented, based on a previously derived self-consistent procedure for obtaining large-scale models for complex system of equations. The model has only a small number of parametrized variables: the small-scale magnetic diffusivity, the scale of the large-scale fields, and a factor in the explicit expression of the αφφ component of the α tensor. Explicit expressions of what corresponds to the other components of the α tensor and of the diffusivity tensor are derived in terms of the large-scale meridional flow and of the differential rotation law, without introducing additional parameters. A very simple simulation of a solar-like dynamo, employing the model without meridional flow shows reasonable magnetic field evolution, with a cycle duration of about 2/3 that of the Sun, shift of the magnetic field from mid-latitudes towards the equator, poleward migration of the radial field at high latitudes, and correct phase relation between radial and azimuthal components. |
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