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
- Institución
- Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
- OAI Identificador
- paperaa:paper_00046361_v426_n3_p1065_Mininni
Ver los metadatos del registro completo
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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/ar2025-09-29T13:42:55Zpaperaa: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:18962025-09-29 13:42:56.448Biblioteca 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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13.070432 |