Helicity analysis for expanding magnetic clouds: A case study

Magnetic Clouds (MCs) are the interplanetary counterpart of coronal mass ejections (CMEs). They transport to the interplanetary medium the magnetic flux and helicity released in CMEs by the Sun. At 1 AU from the Sun, MCs are generally modeled as static flux ropes, i.e., considering them as rigid bod...

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Autores principales: Nakwacki, M.S., Dasso, S., Mandrimi, C.H., Demoalin, P.
Formato: CONF
Materias:
Magnetic clouds
Magnetic helicity
Magnetic properties
Mathematical models
Solar radiation
Magnetic materials
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_03796566_v_n592_p629_Nakwacki
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling todo:paper_03796566_v_n592_p629_Nakwacki2023-10-03T15:33:35Z Helicity analysis for expanding magnetic clouds: A case study Nakwacki, M.S. Dasso, S. Mandrimi, C.H. Demoalin, P. Magnetic clouds Magnetic helicity Magnetic properties Mathematical models Solar radiation Magnetic clouds Magnetic helicity Magnetic materials Magnetic Clouds (MCs) are the interplanetary counterpart of coronal mass ejections (CMEs). They transport to the interplanetary medium the magnetic flux and helicity released in CMEs by the Sun. At 1 AU from the Sun, MCs are generally modeled as static flux ropes, i.e., considering them as rigid bodies traveling through the solar wind. However, the velocity profile of some MCs presents clear signatures of a significant expansion while observed in situ by a spacecraft in the heliosphere. We present here an analysis of the magnetic structure of an expanding magnetic cloud observed during the raising phase of solar cycle 23 by the spacecraft Wind. We consider a dynamical model, based on a self-similar behavior for the cloud radial velocity. We assume a free expansion for the cloud, and a cylindrical linear force free field (i.e., the Lundquist's field) as the initial conditions for its magnetic configuration. We derive theoretical expressions for the magnetic flux, across a surface perpendicular to the cloud axis, and for the magnetic helicity per unit length along the tube using the self-similar model. Finally, we compute these magnitudes fitting the free parameters of the expanding model to in situ magnetic observations, and compare them with those obtained from the linear force free static model. Fil:Nakwacki, M.S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. CONF info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_03796566_v_n592_p629_Nakwacki
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Magnetic clouds
Magnetic helicity
Magnetic properties
Mathematical models
Solar radiation
Magnetic clouds
Magnetic helicity
Magnetic materials
spellingShingle Magnetic clouds
Magnetic helicity
Magnetic properties
Mathematical models
Solar radiation
Magnetic clouds
Magnetic helicity
Magnetic materials
Nakwacki, M.S.
Dasso, S.
Mandrimi, C.H.
Demoalin, P.
Helicity analysis for expanding magnetic clouds: A case study
topic_facet Magnetic clouds
Magnetic helicity
Magnetic properties
Mathematical models
Solar radiation
Magnetic clouds
Magnetic helicity
Magnetic materials
description Magnetic Clouds (MCs) are the interplanetary counterpart of coronal mass ejections (CMEs). They transport to the interplanetary medium the magnetic flux and helicity released in CMEs by the Sun. At 1 AU from the Sun, MCs are generally modeled as static flux ropes, i.e., considering them as rigid bodies traveling through the solar wind. However, the velocity profile of some MCs presents clear signatures of a significant expansion while observed in situ by a spacecraft in the heliosphere. We present here an analysis of the magnetic structure of an expanding magnetic cloud observed during the raising phase of solar cycle 23 by the spacecraft Wind. We consider a dynamical model, based on a self-similar behavior for the cloud radial velocity. We assume a free expansion for the cloud, and a cylindrical linear force free field (i.e., the Lundquist's field) as the initial conditions for its magnetic configuration. We derive theoretical expressions for the magnetic flux, across a surface perpendicular to the cloud axis, and for the magnetic helicity per unit length along the tube using the self-similar model. Finally, we compute these magnitudes fitting the free parameters of the expanding model to in situ magnetic observations, and compare them with those obtained from the linear force free static model.
format CONF
author Nakwacki, M.S.
Dasso, S.
Mandrimi, C.H.
Demoalin, P.
author_facet Nakwacki, M.S.
Dasso, S.
Mandrimi, C.H.
Demoalin, P.
author_sort Nakwacki, M.S.
title Helicity analysis for expanding magnetic clouds: A case study
title_short Helicity analysis for expanding magnetic clouds: A case study
title_full Helicity analysis for expanding magnetic clouds: A case study
title_fullStr Helicity analysis for expanding magnetic clouds: A case study
title_full_unstemmed Helicity analysis for expanding magnetic clouds: A case study
title_sort helicity analysis for expanding magnetic clouds: a case study
url http://hdl.handle.net/20.500.12110/paper_03796566_v_n592_p629_Nakwacki
work_keys_str_mv AT nakwackims helicityanalysisforexpandingmagneticcloudsacasestudy
AT dassos helicityanalysisforexpandingmagneticcloudsacasestudy
AT mandrimich helicityanalysisforexpandingmagneticcloudsacasestudy
AT demoalinp helicityanalysisforexpandingmagneticcloudsacasestudy
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