A new technique for comparing solar dynamo models and observations

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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...

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Detalles Bibliográficos
Autores principales: Mininni, P.D., Gómez, D.O.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2004
Materias:
Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paperaa:paper_00046361_v426_n3_p1065_Mininni2023-06-12T16:40:44Z A new technique for comparing solar dynamo models and observations Astron. Astrophys. 2004;426(3):1065-1073 Mininni, P.D. Gómez, D.O. 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 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. 2004 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language Inglés
orig_language_str_mv eng
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
spellingShingle 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
Mininni, P.D.
Gómez, D.O.
A new technique for comparing solar dynamo models and observations
topic_facet 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
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.
format Artículo
Artículo
publishedVersion
author Mininni, P.D.
Gómez, D.O.
author_facet Mininni, P.D.
Gómez, D.O.
author_sort Mininni, P.D.
title A new technique for comparing solar dynamo models and observations
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 new technique for comparing solar dynamo models and observations
publishDate 2004
url http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
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