The interplanetary magnetic structure that guides solar relativistic particles

Autores
Masson, S.; Démoulin, P.; Dasso, S.; Klein, K.-L.
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral. Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors. Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE. Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts. Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs. © 2012 ESO.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astron. Astrophys. 2012;538
Materia
methods: data analysis
solar-terrestrial relations
Sun: heliosphere
Activity cycles
Arrival time
Energetic particle measurement
Energetic particles
Fast solar winds
High-energy particles
In-situ measurement
Interplanetary coronal mass ejections
Interplanetary magnetic fields
Methods:data analysis
Neutron monitors
Parker spiral
Path length
Pitch-angle scattering
Plasma parameter
Radio bursts
Relativistic particles
Relativistic solar particles
Solar activity
Solar-terrestrial relations
Transient structure
Velocity dispersion
Electron beams
Magnetic bubbles
Magnetic fields
Magnetic structure
Magnetoplasma
Relativity
Solar energy
Solar radiation
Solar system
Solar wind
Interplanetary spacecraft
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_00046361_v538_n_p_Masson

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oai_identifier_str paperaa:paper_00046361_v538_n_p_Masson
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling The interplanetary magnetic structure that guides solar relativistic particlesMasson, S.Démoulin, P.Dasso, S.Klein, K.-L.methods: data analysissolar-terrestrial relationsSun: heliosphereActivity cyclesArrival timeEnergetic particle measurementEnergetic particlesFast solar windsHigh-energy particlesIn-situ measurementInterplanetary coronal mass ejectionsInterplanetary magnetic fieldsMethods:data analysisNeutron monitorsParker spiralPath lengthPitch-angle scatteringPlasma parameterRadio burstsRelativistic particlesRelativistic solar particlesSolar activitySolar-terrestrial relationsTransient structureVelocity dispersionElectron beamsMagnetic bubblesMagnetic fieldsMagnetic structureMagnetoplasmaRelativitySolar energySolar radiationSolar systemSolar windInterplanetary spacecraftContext. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral. Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors. Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE. Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts. Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs. © 2012 ESO.Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.2012info: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_v538_n_p_MassonAstron. Astrophys. 2012;538reponame: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/ar2025-09-29T13:42:54Zpaperaa:paper_00046361_v538_n_p_MassonInstitucionalhttps://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 13:42:56.163Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv The interplanetary magnetic structure that guides solar relativistic particles
title The interplanetary magnetic structure that guides solar relativistic particles
spellingShingle The interplanetary magnetic structure that guides solar relativistic particles
Masson, S.
methods: data analysis
solar-terrestrial relations
Sun: heliosphere
Activity cycles
Arrival time
Energetic particle measurement
Energetic particles
Fast solar winds
High-energy particles
In-situ measurement
Interplanetary coronal mass ejections
Interplanetary magnetic fields
Methods:data analysis
Neutron monitors
Parker spiral
Path length
Pitch-angle scattering
Plasma parameter
Radio bursts
Relativistic particles
Relativistic solar particles
Solar activity
Solar-terrestrial relations
Transient structure
Velocity dispersion
Electron beams
Magnetic bubbles
Magnetic fields
Magnetic structure
Magnetoplasma
Relativity
Solar energy
Solar radiation
Solar system
Solar wind
Interplanetary spacecraft
title_short The interplanetary magnetic structure that guides solar relativistic particles
title_full The interplanetary magnetic structure that guides solar relativistic particles
title_fullStr The interplanetary magnetic structure that guides solar relativistic particles
title_full_unstemmed The interplanetary magnetic structure that guides solar relativistic particles
title_sort The interplanetary magnetic structure that guides solar relativistic particles
dc.creator.none.fl_str_mv Masson, S.
Démoulin, P.
Dasso, S.
Klein, K.-L.
author Masson, S.
author_facet Masson, S.
Démoulin, P.
Dasso, S.
Klein, K.-L.
author_role author
author2 Démoulin, P.
Dasso, S.
Klein, K.-L.
author2_role author
author
author
dc.subject.none.fl_str_mv methods: data analysis
solar-terrestrial relations
Sun: heliosphere
Activity cycles
Arrival time
Energetic particle measurement
Energetic particles
Fast solar winds
High-energy particles
In-situ measurement
Interplanetary coronal mass ejections
Interplanetary magnetic fields
Methods:data analysis
Neutron monitors
Parker spiral
Path length
Pitch-angle scattering
Plasma parameter
Radio bursts
Relativistic particles
Relativistic solar particles
Solar activity
Solar-terrestrial relations
Transient structure
Velocity dispersion
Electron beams
Magnetic bubbles
Magnetic fields
Magnetic structure
Magnetoplasma
Relativity
Solar energy
Solar radiation
Solar system
Solar wind
Interplanetary spacecraft
topic methods: data analysis
solar-terrestrial relations
Sun: heliosphere
Activity cycles
Arrival time
Energetic particle measurement
Energetic particles
Fast solar winds
High-energy particles
In-situ measurement
Interplanetary coronal mass ejections
Interplanetary magnetic fields
Methods:data analysis
Neutron monitors
Parker spiral
Path length
Pitch-angle scattering
Plasma parameter
Radio bursts
Relativistic particles
Relativistic solar particles
Solar activity
Solar-terrestrial relations
Transient structure
Velocity dispersion
Electron beams
Magnetic bubbles
Magnetic fields
Magnetic structure
Magnetoplasma
Relativity
Solar energy
Solar radiation
Solar system
Solar wind
Interplanetary spacecraft
dc.description.none.fl_txt_mv Context. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral. Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors. Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE. Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts. Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs. © 2012 ESO.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
description Context. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral. Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors. Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE. Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts. Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs. © 2012 ESO.
publishDate 2012
dc.date.none.fl_str_mv 2012
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_v538_n_p_Masson
url http://hdl.handle.net/20.500.12110/paper_00046361_v538_n_p_Masson
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. 2012;538
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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