Toward a dynamo model for the solar tachocline
The generation of magnetic field on the Sun is caused by a dynamo mechanism, and is related with the differential rotation of the solar interior. Helioseismologic observations show that strong velocity gradients concentrate in a thin layer located at the base of the convective region, known as the t...
| Autores: | , , |
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| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2005 |
| País: | Argentina |
| Recursos: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositório: | CONICET Digital (CONICET) |
| Idioma: | inglês |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/22058 |
| Acesso em linha: | http://hdl.handle.net/11336/22058 |
| Access Level: | Acceso aberto |
| Palavra-chave: | https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Resumo: | The generation of magnetic field on the Sun is caused by a dynamo mechanism, and is related with the differential rotation of the solar interior. Helioseismologic observations show that strong velocity gradients concentrate in a thin layer located at the base of the convective region, known as the tachocline. This remarkable observational finding lends support to a theoretical model for the solar dynamo, based on a magnetohydrodynamic extension of the so called shallow water approximation. We developed a numerical code to integrate the dynamic equations. Our analysis shows an initial stage during which the magnetic energy grows exponentially fast. In a subsequent stage we find that magnetic energy keeps growing until it reaches equipartition with the mechanical energy of the flow. |
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