Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU

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Context. Significant quantities of magnetized plasma are transported from the Sun to the interstellar medium via interplanetary coronal mass ejections (ICMEs). Magnetic clouds (MCs) are a particular subset of ICMEs, forming large-scale magnetic flux ropes. Their evolution in the solar wind is comple...

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Autores principales: Nakwacki, M.S., Dasso, S., Démoulin, P., Mandrini, C.H., Gulisano, A.M.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2011
Materias:
Magnetic fields
Magnetohydrodynamics (MHD)
Solar wind
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: magnetic topology
Cross section
Dynamical evolution
Expansion rate
Flux ropes
Global quantities
Helicities
In-situ observations
Interplanetary coronal mass ejections
Interplanetary medium
Interstellar mediums
Link structure
Magnetic clouds
Magnetic configuration
Magnetic energies
Magnetic flux ropes
Magnetic force
Magnetic-field intensity
Magnetized plasmas
Mass densities
Radial direction
Solar source
Surrounding environment
Velocity profiles
Aspect ratio
Clouds
Expansion
Interplanetary spacecraft
Magnetic flux
Magnetoplasma
Planetary surface analysis
Solar system
Wind
Magnetohydrodynamics
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v535_n_p_Nakwacki
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paperaa:paper_00046361_v535_n_p_Nakwacki2023-06-12T16:40:53Z Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU Astron. Astrophys. 2011;535 Nakwacki, M.S. Dasso, S. Démoulin, P. Mandrini, C.H. Gulisano, A.M. Magnetic fields Magnetohydrodynamics (MHD) Solar wind Sun: coronal mass ejections (CMEs) Sun: heliosphere Sun: magnetic topology Cross section Dynamical evolution Expansion rate Flux ropes Global quantities Helicities In-situ observations Interplanetary coronal mass ejections Interplanetary medium Interstellar mediums Link structure Magnetic clouds Magnetic configuration Magnetic energies Magnetic flux ropes Magnetic force Magnetic-field intensity Magnetized plasmas Magnetohydrodynamics (MHD) Mass densities Radial direction Solar source Sun: coronal mass ejections (CMEs) Surrounding environment Velocity profiles Aspect ratio Clouds Expansion Interplanetary spacecraft Magnetic fields Magnetic flux Magnetoplasma Planetary surface analysis Solar system Solar wind Wind Magnetohydrodynamics Context. Significant quantities of magnetized plasma are transported from the Sun to the interstellar medium via interplanetary coronal mass ejections (ICMEs). Magnetic clouds (MCs) are a particular subset of ICMEs, forming large-scale magnetic flux ropes. Their evolution in the solar wind is complex and mainly determined by their own magnetic forces and the interaction with the surrounding solar wind. Aims. Magnetic clouds are strongly affected by the surrounding environment as they evolve in the solar wind. We study expansion of MCs, its consequent decrease in magnetic field intensity and mass density, and the possible evolution of the so-called global ideal-MHD invariants. Methods. In this work we analyze the evolution of a particular MC (observed in March 1998) using in situ observations made by two spacecraft approximately aligned with the Sun, the first one at 1 AU from the Sun and the second one at 5.4 AU. We describe the magnetic configuration of the MC using different models and compute relevant global quantities (magnetic fluxes, helicity, and energy) at both heliodistances. We also tracked this structure back to the Sun, to find out its solar source. Results. We find that the flux rope is significantly distorted at 5.4 AU. From the observed decay of magnetic field and mass density, we quantify how anisotropic is the expansion and the consequent deformation of the flux rope in favor of a cross section with an aspect ratio at 5.4 AU of ≈ 1.6 (larger in the direction perpendicular to the radial direction from the Sun). We quantify the ideal-MHD invariants and magnetic energy at both locations, and find that invariants are almost conserved, while the magnetic energy decays as expected with the expansion rate found. Conclusions. The use of MHD invariants to link structures at the Sun and the interplanetary medium is supported by the results of this multi-spacecraft study. We also conclude that the local dimensionless expansion rate, which is computed from the velocity profile observed by a single-spacecraft, is very accurate for predicting the evolution of flux ropes in the solar wind. © 2011 ESO. 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. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Gulisano, A.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2011 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_v535_n_p_Nakwacki
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 Magnetic fields
Magnetohydrodynamics (MHD)
Solar wind
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: magnetic topology
Cross section
Dynamical evolution
Expansion rate
Flux ropes
Global quantities
Helicities
In-situ observations
Interplanetary coronal mass ejections
Interplanetary medium
Interstellar mediums
Link structure
Magnetic clouds
Magnetic configuration
Magnetic energies
Magnetic flux ropes
Magnetic force
Magnetic-field intensity
Magnetized plasmas
Magnetohydrodynamics (MHD)
Mass densities
Radial direction
Solar source
Sun: coronal mass ejections (CMEs)
Surrounding environment
Velocity profiles
Aspect ratio
Clouds
Expansion
Interplanetary spacecraft
Magnetic fields
Magnetic flux
Magnetoplasma
Planetary surface analysis
Solar system
Solar wind
Wind
Magnetohydrodynamics
spellingShingle Magnetic fields
Magnetohydrodynamics (MHD)
Solar wind
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: magnetic topology
Cross section
Dynamical evolution
Expansion rate
Flux ropes
Global quantities
Helicities
In-situ observations
Interplanetary coronal mass ejections
Interplanetary medium
Interstellar mediums
Link structure
Magnetic clouds
Magnetic configuration
Magnetic energies
Magnetic flux ropes
Magnetic force
Magnetic-field intensity
Magnetized plasmas
Magnetohydrodynamics (MHD)
Mass densities
Radial direction
Solar source
Sun: coronal mass ejections (CMEs)
Surrounding environment
Velocity profiles
Aspect ratio
Clouds
Expansion
Interplanetary spacecraft
Magnetic fields
Magnetic flux
Magnetoplasma
Planetary surface analysis
Solar system
Solar wind
Wind
Magnetohydrodynamics
Nakwacki, M.S.
Dasso, S.
Démoulin, P.
Mandrini, C.H.
Gulisano, A.M.
Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
topic_facet Magnetic fields
Magnetohydrodynamics (MHD)
Solar wind
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: magnetic topology
Cross section
Dynamical evolution
Expansion rate
Flux ropes
Global quantities
Helicities
In-situ observations
Interplanetary coronal mass ejections
Interplanetary medium
Interstellar mediums
Link structure
Magnetic clouds
Magnetic configuration
Magnetic energies
Magnetic flux ropes
Magnetic force
Magnetic-field intensity
Magnetized plasmas
Magnetohydrodynamics (MHD)
Mass densities
Radial direction
Solar source
Sun: coronal mass ejections (CMEs)
Surrounding environment
Velocity profiles
Aspect ratio
Clouds
Expansion
Interplanetary spacecraft
Magnetic fields
Magnetic flux
Magnetoplasma
Planetary surface analysis
Solar system
Solar wind
Wind
Magnetohydrodynamics
description Context. Significant quantities of magnetized plasma are transported from the Sun to the interstellar medium via interplanetary coronal mass ejections (ICMEs). Magnetic clouds (MCs) are a particular subset of ICMEs, forming large-scale magnetic flux ropes. Their evolution in the solar wind is complex and mainly determined by their own magnetic forces and the interaction with the surrounding solar wind. Aims. Magnetic clouds are strongly affected by the surrounding environment as they evolve in the solar wind. We study expansion of MCs, its consequent decrease in magnetic field intensity and mass density, and the possible evolution of the so-called global ideal-MHD invariants. Methods. In this work we analyze the evolution of a particular MC (observed in March 1998) using in situ observations made by two spacecraft approximately aligned with the Sun, the first one at 1 AU from the Sun and the second one at 5.4 AU. We describe the magnetic configuration of the MC using different models and compute relevant global quantities (magnetic fluxes, helicity, and energy) at both heliodistances. We also tracked this structure back to the Sun, to find out its solar source. Results. We find that the flux rope is significantly distorted at 5.4 AU. From the observed decay of magnetic field and mass density, we quantify how anisotropic is the expansion and the consequent deformation of the flux rope in favor of a cross section with an aspect ratio at 5.4 AU of ≈ 1.6 (larger in the direction perpendicular to the radial direction from the Sun). We quantify the ideal-MHD invariants and magnetic energy at both locations, and find that invariants are almost conserved, while the magnetic energy decays as expected with the expansion rate found. Conclusions. The use of MHD invariants to link structures at the Sun and the interplanetary medium is supported by the results of this multi-spacecraft study. We also conclude that the local dimensionless expansion rate, which is computed from the velocity profile observed by a single-spacecraft, is very accurate for predicting the evolution of flux ropes in the solar wind. © 2011 ESO.
format Artículo
Artículo
publishedVersion
author Nakwacki, M.S.
Dasso, S.
Démoulin, P.
Mandrini, C.H.
Gulisano, A.M.
author_facet Nakwacki, M.S.
Dasso, S.
Démoulin, P.
Mandrini, C.H.
Gulisano, A.M.
author_sort Nakwacki, M.S.
title Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
title_short Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
title_full Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
title_fullStr Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
title_full_unstemmed Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU
title_sort dynamical evolution of a magnetic cloud from the sun to 5.4 au
publishDate 2011
url http://hdl.handle.net/20.500.12110/paper_00046361_v535_n_p_Nakwacki
work_keys_str_mv AT nakwackims dynamicalevolutionofamagneticcloudfromthesunto54au
AT dassos dynamicalevolutionofamagneticcloudfromthesunto54au
AT demoulinp dynamicalevolutionofamagneticcloudfromthesunto54au
AT mandrinich dynamicalevolutionofamagneticcloudfromthesunto54au
AT gulisanoam dynamicalevolutionofamagneticcloudfromthesunto54au
_version_ 1769810066350800896

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