Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models

Context. By coupling the EUropean Heliospheric FORcasting Information Asset (EUHFORIA) and the improved Particle Acceleration and Transport in the Heliosphere (iPATH) models, we model two energetic storm particle (ESP) events originating from the same active region (AR 13088) and observed by Solar O...

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Autores: Ding, Zheyi, Li, Gang, Mason, G. M., Poedts, Stefaan, Kouloumvakos, Athanasios, Ho, George C., Wijsen, Nicolas, Wimmer-Schweingrube, F., Rodríguez-Pacheco Martín, Javier|||0000-0002-4240-1115
Tipo de recurso: artículo
Fecha de publicación:2024
País:España
Institución:Universidad de Alcalá (UAH)
Repositorio:e_Buah Biblioteca Digital Universidad de Alcalá
Idioma:inglés
OAI Identifier:oai:ebuah.uah.es:10017/68250
Acceso en línea:http://hdl.handle.net/10017/68250
https://dx.doi.org/10.1051/0004-6361/202347506
Access Level:acceso abierto
Palabra clave:Acceleration of particles
Shock waves
Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: particle emission
Astronomía
Astronomy
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spelling Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH modelsDing, ZheyiLi, GangMason, G. M.Poedts, StefaanKouloumvakos, AthanasiosHo, George C.Wijsen, NicolasWimmer-Schweingrube, F.Rodríguez-Pacheco Martín, Javier|||0000-0002-4240-1115Acceleration of particlesShock wavesSun: coronaSun: coronal mass ejections (CMEs)Sun: heliosphereSun: particle emissionAstronomíaAstronomyContext. By coupling the EUropean Heliospheric FORcasting Information Asset (EUHFORIA) and the improved Particle Acceleration and Transport in the Heliosphere (iPATH) models, we model two energetic storm particle (ESP) events originating from the same active region (AR 13088) and observed by Solar Orbiter (SolO) on August 31, 2022, and September 5, 2022.Aims. By combining numerical simulations and SolO observations, we aim to better understand particle acceleration and the transport process in the inner heliosphere.Methods. We simulated two coronal mass ejections (CMEs) in a data-driven, real-time solar wind background with the EUHFORIA code. The MHD parameters concerning the shock and downstream medium were computed from EUHFORIA as inputs for the iPATH model. In the iPATH model, a shell structure was maintained to model the turbulence-enhanced shock sheath. At the shock front, assuming diffuse shock acceleration, the particle distribution was obtained by taking the steady state solution with the instantaneous shock parameters. Upstream of the shock, particles escape, and their transport in the solar wind was described by a focused transport equation using the backward stochastic differential equation method.Results. While both events originated from the same active region, they exhibited notable differences. One notable difference is the duration of the events, as the August ESP event lasted for 7 h, while the September event persisted for 16 h. Another key difference concerns the time intensity profiles. The September event showed a clear crossover upstream of the shock where the intensity of higher energy protons exceeds those of lower energy protons, leading to positive ("reverse") spectral indices prior to the shock passage. For both events, our simulations replicate the observed duration of the shock sheath, depending on the deceleration history of the CME. Imposing different choices of escaping length scale, which is related to the decay of upstream turbulence, the modelled time intensity profiles prior to the shock arrival also agree with observations. In particular, the crossover of this time profile in the September event is well reproduced. We show that a "reverse" upstream spectrum is the result of the interplay between two length scales. One characterizes the decay of the accelerated particles upstream of the shock, which are controlled by the energy-dependent diffusion coefficient, and the other characterizes the decay of upstream turbulence power, which is related to the process of how streaming protons upstream of the shock excite Alfven waves.Conclusions. The behavior of solar energetic particle (SEP) events depends on many variables. Even similar eruptions from the same AR may lead to SEP events that have very different characteristics. Simulations taking into account real-time background solar wind, the dynamics of the CME propagation, and upstream turbulence at the shock front are necessary to thoroughly understand the ESP phase of large SEP events.EDP Sciences20242024-01-22journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10017/68250https://dx.doi.org/10.1051/0004-6361/202347506reponame:e_Buah Biblioteca Digital Universidad de Alcaláinstname:Universidad de Alcalá (UAH)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution 4.0 Internationalhttp://creativecommons.org/licenses/by/4.0/info:eu-repo/semantics/openAccessoai:ebuah.uah.es:10017/682502026-06-18T11:13:07Z
dc.title.none.fl_str_mv Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
title Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
spellingShingle Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
Ding, Zheyi
Acceleration of particles
Shock waves
Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: particle emission
Astronomía
Astronomy
title_short Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
title_full Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
title_fullStr Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
title_full_unstemmed Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
title_sort Modelling two energetic storm particle events observed by Solar Orbiter using the combined EUHFORIA and iPATH models
dc.creator.none.fl_str_mv Ding, Zheyi
Li, Gang
Mason, G. M.
Poedts, Stefaan
Kouloumvakos, Athanasios
Ho, George C.
Wijsen, Nicolas
Wimmer-Schweingrube, F.
Rodríguez-Pacheco Martín, Javier|||0000-0002-4240-1115
author Ding, Zheyi
author_facet Ding, Zheyi
Li, Gang
Mason, G. M.
Poedts, Stefaan
Kouloumvakos, Athanasios
Ho, George C.
Wijsen, Nicolas
Wimmer-Schweingrube, F.
Rodríguez-Pacheco Martín, Javier|||0000-0002-4240-1115
author_role author
author2 Li, Gang
Mason, G. M.
Poedts, Stefaan
Kouloumvakos, Athanasios
Ho, George C.
Wijsen, Nicolas
Wimmer-Schweingrube, F.
Rodríguez-Pacheco Martín, Javier|||0000-0002-4240-1115
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Acceleration of particles
Shock waves
Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: particle emission
Astronomía
Astronomy
topic Acceleration of particles
Shock waves
Sun: corona
Sun: coronal mass ejections (CMEs)
Sun: heliosphere
Sun: particle emission
Astronomía
Astronomy
description Context. By coupling the EUropean Heliospheric FORcasting Information Asset (EUHFORIA) and the improved Particle Acceleration and Transport in the Heliosphere (iPATH) models, we model two energetic storm particle (ESP) events originating from the same active region (AR 13088) and observed by Solar Orbiter (SolO) on August 31, 2022, and September 5, 2022.Aims. By combining numerical simulations and SolO observations, we aim to better understand particle acceleration and the transport process in the inner heliosphere.Methods. We simulated two coronal mass ejections (CMEs) in a data-driven, real-time solar wind background with the EUHFORIA code. The MHD parameters concerning the shock and downstream medium were computed from EUHFORIA as inputs for the iPATH model. In the iPATH model, a shell structure was maintained to model the turbulence-enhanced shock sheath. At the shock front, assuming diffuse shock acceleration, the particle distribution was obtained by taking the steady state solution with the instantaneous shock parameters. Upstream of the shock, particles escape, and their transport in the solar wind was described by a focused transport equation using the backward stochastic differential equation method.Results. While both events originated from the same active region, they exhibited notable differences. One notable difference is the duration of the events, as the August ESP event lasted for 7 h, while the September event persisted for 16 h. Another key difference concerns the time intensity profiles. The September event showed a clear crossover upstream of the shock where the intensity of higher energy protons exceeds those of lower energy protons, leading to positive ("reverse") spectral indices prior to the shock passage. For both events, our simulations replicate the observed duration of the shock sheath, depending on the deceleration history of the CME. Imposing different choices of escaping length scale, which is related to the decay of upstream turbulence, the modelled time intensity profiles prior to the shock arrival also agree with observations. In particular, the crossover of this time profile in the September event is well reproduced. We show that a "reverse" upstream spectrum is the result of the interplay between two length scales. One characterizes the decay of the accelerated particles upstream of the shock, which are controlled by the energy-dependent diffusion coefficient, and the other characterizes the decay of upstream turbulence power, which is related to the process of how streaming protons upstream of the shock excite Alfven waves.Conclusions. The behavior of solar energetic particle (SEP) events depends on many variables. Even similar eruptions from the same AR may lead to SEP events that have very different characteristics. Simulations taking into account real-time background solar wind, the dynamics of the CME propagation, and upstream turbulence at the shock front are necessary to thoroughly understand the ESP phase of large SEP events.
publishDate 2024
dc.date.none.fl_str_mv 2024
2024-01-22
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
NA
http://purl.org/coar/version/c_be7fb7dd8ff6fe43
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10017/68250
https://dx.doi.org/10.1051/0004-6361/202347506
url http://hdl.handle.net/10017/68250
https://dx.doi.org/10.1051/0004-6361/202347506
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Attribution 4.0 International
http://creativecommons.org/licenses/by/4.0/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:e_Buah Biblioteca Digital Universidad de Alcalá
instname:Universidad de Alcalá (UAH)
instname_str Universidad de Alcalá (UAH)
reponame_str e_Buah Biblioteca Digital Universidad de Alcalá
collection e_Buah Biblioteca Digital Universidad de Alcalá
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,81155

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