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...

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Autores principales: Lillo, R., Mininni, P.D., Gómez, D.O.
Formato: JOUR
Materias:
Dynamo theories
Magnetic fields
Sun
Approximation theory
Heat convection
Magnetohydrodynamics
Mathematical models
Velocity
Helioseismology
Magnetic energy
Solar dynamo
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_03784371_v349_n3-4_p667_Lillo
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_03784371_v349_n3-4_p667_Lillo
record_format dspace
spelling todo:paper_03784371_v349_n3-4_p667_Lillo2023-10-03T15:32:44Z Toward a dynamo model for the solar tachocline Lillo, R. Mininni, P.D. Gómez, D.O. Dynamo theories Magnetic fields Sun Approximation theory Heat convection Magnetic fields Magnetohydrodynamics Mathematical models Velocity Dynamo theories Helioseismology Magnetic energy Solar dynamo Sun 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. © 2004 Elsevier B.V. All rights reserved. Fil:Lillo, R. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Mininni, P.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_03784371_v349_n3-4_p667_Lillo
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Dynamo theories
Magnetic fields
Sun
Approximation theory
Heat convection
Magnetic fields
Magnetohydrodynamics
Mathematical models
Velocity
Dynamo theories
Helioseismology
Magnetic energy
Solar dynamo
Sun
spellingShingle Dynamo theories
Magnetic fields
Sun
Approximation theory
Heat convection
Magnetic fields
Magnetohydrodynamics
Mathematical models
Velocity
Dynamo theories
Helioseismology
Magnetic energy
Solar dynamo
Sun
Lillo, R.
Mininni, P.D.
Gómez, D.O.
Toward a dynamo model for the solar tachocline
topic_facet Dynamo theories
Magnetic fields
Sun
Approximation theory
Heat convection
Magnetic fields
Magnetohydrodynamics
Mathematical models
Velocity
Dynamo theories
Helioseismology
Magnetic energy
Solar dynamo
Sun
description 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. © 2004 Elsevier B.V. All rights reserved.
format JOUR
author Lillo, R.
Mininni, P.D.
Gómez, D.O.
author_facet Lillo, R.
Mininni, P.D.
Gómez, D.O.
author_sort Lillo, R.
title Toward a dynamo model for the solar tachocline
title_short Toward a dynamo model for the solar tachocline
title_full Toward a dynamo model for the solar tachocline
title_fullStr Toward a dynamo model for the solar tachocline
title_full_unstemmed Toward a dynamo model for the solar tachocline
title_sort toward a dynamo model for the solar tachocline
url http://hdl.handle.net/20.500.12110/paper_03784371_v349_n3-4_p667_Lillo
work_keys_str_mv AT lillor towardadynamomodelforthesolartachocline
AT mininnipd towardadynamomodelforthesolartachocline
AT gomezdo towardadynamomodelforthesolartachocline
_version_ 1807315876131635200

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