A new technique for comparing solar dynamo models and observations

Autores
Mininni, P.D.; Gómez, D.O.
Año de publicación
2004
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years.
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.
Fuente
Astron. Astrophys. 2004;426(3):1065-1073
Materia
Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun: magnetic fields
Sun: sunspots
Sun
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_00046361_v426_n3_p1065_Mininni
Acceder
id BDUBAFCEN_435613fdf862ccc46e41890e8de525ac
oai_identifier_str paperaa:paper_00046361_v426_n3_p1065_Mininni
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling A new technique for comparing solar dynamo models and observationsMininni, P.D.Gómez, D.O.Magnetohydrodynamics (MHD)Sun: magnetic fieldsSun: sunspotsAstrophysicsChaos theoryKinematicsMagnetic fieldsMagnetohydrodynamicsRandom processesSatellite observatoriesSpectroscopySolar cycleStochasticitySun: magnetic fieldsSun: sunspotsSunWe present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years.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.2004info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_MininniAstron. Astrophys. 2004;426(3):1065-1073reponame:Biblioteca Digital (UBA-FCEN)instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesinstacron:UBA-FCENenginfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/2.5/ar2025-11-06T09:39:40Zpaperaa:paper_00046361_v426_n3_p1065_MininniInstitucionalhttps://digital.bl.fcen.uba.ar/Universidad públicaNo correspondehttps://digital.bl.fcen.uba.ar/cgi-bin/oaiserver.cgiana@bl.fcen.uba.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:18962025-11-06 09:39:42.195Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv A new technique for comparing solar dynamo models and observations
title A new technique for comparing solar dynamo models and observations
spellingShingle A new technique for comparing solar dynamo models and observations
Mininni, P.D.
Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun: magnetic fields
Sun: sunspots
Sun
title_short A new technique for comparing solar dynamo models and observations
title_full A new technique for comparing solar dynamo models and observations
title_fullStr A new technique for comparing solar dynamo models and observations
title_full_unstemmed A new technique for comparing solar dynamo models and observations
title_sort A new technique for comparing solar dynamo models and observations
dc.creator.none.fl_str_mv Mininni, P.D.
Gómez, D.O.
author Mininni, P.D.
author_facet Mininni, P.D.
Gómez, D.O.
author_role author
author2 Gómez, D.O.
author2_role author
dc.subject.none.fl_str_mv Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun: magnetic fields
Sun: sunspots
Sun
topic Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun: magnetic fields
Sun: sunspots
Sun
dc.description.none.fl_txt_mv We present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years.
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.
description We present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years.
publishDate 2004
dc.date.none.fl_str_mv 2004
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
url http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
dc.language.none.fl_str_mv eng
language eng
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/2.5/ar
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/2.5/ar
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv Astron. Astrophys. 2004;426(3):1065-1073
reponame:Biblioteca Digital (UBA-FCEN)
instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron:UBA-FCEN
reponame_str Biblioteca Digital (UBA-FCEN)
collection Biblioteca Digital (UBA-FCEN)
instname_str Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron_str UBA-FCEN
institution UBA-FCEN
repository.name.fl_str_mv Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
repository.mail.fl_str_mv ana@bl.fcen.uba.ar
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score 12.976206

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