The interplanetary magnetic structure that guides solar relativistic particles

Mostrar todas las versiones(3)

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 tran...

Descripción completa

Guardado en:
Detalles Bibliográficos
Autores principales: Masson, S., Démoulin, P., Dasso, S., Klein, K.-L.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2012
Materias:
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
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v538_n_p_Masson
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paperaa:paper_00046361_v538_n_p_Masson
record_format dspace
spelling paperaa:paper_00046361_v538_n_p_Masson2023-06-12T16:40:53Z The interplanetary magnetic structure that guides solar relativistic particles Astron. Astrophys. 2012;538 Masson, S. Démoulin, P. Dasso, S. Klein, K.-L. 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 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. 2012 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_v538_n_p_Masson
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 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
spellingShingle 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
Masson, S.
Démoulin, P.
Dasso, S.
Klein, K.-L.
The interplanetary magnetic structure that guides solar relativistic particles
topic_facet 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
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.
format Artículo
Artículo
publishedVersion
author Masson, S.
Démoulin, P.
Dasso, S.
Klein, K.-L.
author_facet Masson, S.
Démoulin, P.
Dasso, S.
Klein, K.-L.
author_sort Masson, S.
title The interplanetary magnetic structure that guides solar relativistic particles
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 interplanetary magnetic structure that guides solar relativistic particles
publishDate 2012
url http://hdl.handle.net/20.500.12110/paper_00046361_v538_n_p_Masson
work_keys_str_mv AT massons theinterplanetarymagneticstructurethatguidessolarrelativisticparticles
AT demoulinp theinterplanetarymagneticstructurethatguidessolarrelativisticparticles
AT dassos theinterplanetarymagneticstructurethatguidessolarrelativisticparticles
AT kleinkl theinterplanetarymagneticstructurethatguidessolarrelativisticparticles
AT massons interplanetarymagneticstructurethatguidessolarrelativisticparticles
AT demoulinp interplanetarymagneticstructurethatguidessolarrelativisticparticles
AT dassos interplanetarymagneticstructurethatguidessolarrelativisticparticles
AT kleinkl interplanetarymagneticstructurethatguidessolarrelativisticparticles
_version_ 1769810066559467520

Ejemplares similares