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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Autores principales:	Mininni, P.D., Gómez, D.O.
Formato:	JOUR
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

id	todo:paper_00046361_v426_n3_p1065_Mininni
record_format	dspace
spelling	todo:paper_00046361_v426_n3_p1065_Mininni2023-10-03T14:00:09Z A new technique for comparing solar dynamo models and observations 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. JOUR 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)
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	JOUR
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
url	http://hdl.handle.net/20.500.12110/paper_00046361_v426_n3_p1065_Mininni
work_keys_str_mv	AT mininnipd anewtechniqueforcomparingsolardynamomodelsandobservations AT gomezdo anewtechniqueforcomparingsolardynamomodelsandobservations AT mininnipd newtechniqueforcomparingsolardynamomodelsandobservations AT gomezdo newtechniqueforcomparingsolardynamomodelsandobservations
_version_	1807314998691627008

A new technique for comparing solar dynamo models and observations

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