A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream

Solar wind stream interaction regions (SIRs) are often characterized by energetic ion enhancements. The mechanisms accelerating these particles, as well as the locations where the acceleration occurs, remain debated. Here, we report the findings of a simulation of a SIR event observed by Parker Sola...

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Autores: Wijsen, Nicolas, Samara, Evangelia, Aran i Sensat, Maria dels Àngels, Lario, David, Pomoell, Jens, Poedts, Stefaan
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:España
Institución:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
Repositorio:Recercat. Dipósit de la Recerca de Catalunya
OAI Identifier:oai:recercat.cat:2445/175335
Acceso en línea:https://hdl.handle.net/2445/175335
Access Level:acceso abierto
Palabra clave:Vent solar
Acceleradors de partícules
Solar wind
Particle accelerators
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spelling A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind streamWijsen, NicolasSamara, EvangeliaAran i Sensat, Maria dels ÀngelsLario, DavidPomoell, JensPoedts, StefaanVent solarAcceleradors de partículesSolar windParticle acceleratorsSolar wind stream interaction regions (SIRs) are often characterized by energetic ion enhancements. The mechanisms accelerating these particles, as well as the locations where the acceleration occurs, remain debated. Here, we report the findings of a simulation of a SIR event observed by Parker Solar Probe at ~0.56 au and the Solar Terrestrial Relations Observatory-Ahead at ~0.95 au in 2019 September when both spacecraft were approximately radially aligned with the Sun. The simulation reproduces the solar wind configuration and the energetic particle enhancements observed by both spacecraft. Our results show that the energetic particles are produced at the compression waves associated with the SIR and that the suprathermal tail of the solar wind is a good candidate to provide the seed population for particle acceleration. The simulation confirms that the acceleration process does not require shock waves and can already commence within Earth's orbit, with an energy dependence on the precise location where particles are accelerated. The three-dimensional configuration of the solar wind streams strongly modulates the energetic particle distributions, illustrating the necessity of advanced models to understand these particle events.Institute of Physics (IOP)2021202120212021info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersion12 p.application/pdfhttps://hdl.handle.net/2445/175335Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Recercat. Dipósit de la Recerca de Catalunyainstname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)InglésReproducció del document publicat a: https://doi.org/10.3847/2041-8213/abe1cbAstrophysical Journal Letters, 2021, vol. 908, num. 2https://doi.org/10.3847/2041-8213/abe1cbinfo:eu-repo/grantAgreement/EC/H2020/870405(c) American Astronomical Society, 2021info:eu-repo/semantics/openAccessoai:recercat.cat:2445/1753352026-05-29T05:05:01Z
dc.title.none.fl_str_mv A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
title A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
spellingShingle A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
Wijsen, Nicolas
Vent solar
Acceleradors de partícules
Solar wind
Particle accelerators
title_short A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
title_full A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
title_fullStr A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
title_full_unstemmed A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
title_sort A Self-consistent simulation of proton acceleration and transport near a high-speed solar wind stream
dc.creator.none.fl_str_mv Wijsen, Nicolas
Samara, Evangelia
Aran i Sensat, Maria dels Àngels
Lario, David
Pomoell, Jens
Poedts, Stefaan
author Wijsen, Nicolas
author_facet Wijsen, Nicolas
Samara, Evangelia
Aran i Sensat, Maria dels Àngels
Lario, David
Pomoell, Jens
Poedts, Stefaan
author_role author
author2 Samara, Evangelia
Aran i Sensat, Maria dels Àngels
Lario, David
Pomoell, Jens
Poedts, Stefaan
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv Vent solar
Acceleradors de partícules
Solar wind
Particle accelerators
topic Vent solar
Acceleradors de partícules
Solar wind
Particle accelerators
description Solar wind stream interaction regions (SIRs) are often characterized by energetic ion enhancements. The mechanisms accelerating these particles, as well as the locations where the acceleration occurs, remain debated. Here, we report the findings of a simulation of a SIR event observed by Parker Solar Probe at ~0.56 au and the Solar Terrestrial Relations Observatory-Ahead at ~0.95 au in 2019 September when both spacecraft were approximately radially aligned with the Sun. The simulation reproduces the solar wind configuration and the energetic particle enhancements observed by both spacecraft. Our results show that the energetic particles are produced at the compression waves associated with the SIR and that the suprathermal tail of the solar wind is a good candidate to provide the seed population for particle acceleration. The simulation confirms that the acceleration process does not require shock waves and can already commence within Earth's orbit, with an energy dependence on the precise location where particles are accelerated. The three-dimensional configuration of the solar wind streams strongly modulates the energetic particle distributions, illustrating the necessity of advanced models to understand these particle events.
publishDate 2021
dc.date.none.fl_str_mv 2021
2021
2021
2021
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv https://hdl.handle.net/2445/175335
url https://hdl.handle.net/2445/175335
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv Reproducció del document publicat a: https://doi.org/10.3847/2041-8213/abe1cb
Astrophysical Journal Letters, 2021, vol. 908, num. 2
https://doi.org/10.3847/2041-8213/abe1cb
info:eu-repo/grantAgreement/EC/H2020/870405
dc.rights.none.fl_str_mv (c) American Astronomical Society, 2021
info:eu-repo/semantics/openAccess
rights_invalid_str_mv (c) American Astronomical Society, 2021
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 12 p.
application/pdf
dc.publisher.none.fl_str_mv Institute of Physics (IOP)
publisher.none.fl_str_mv Institute of Physics (IOP)
dc.source.none.fl_str_mv Articles publicats en revistes (Física Quàntica i Astrofísica)
reponame:Recercat. Dipósit de la Recerca de Catalunya
instname:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
instname_str Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
reponame_str Recercat. Dipósit de la Recerca de Catalunya
collection Recercat. Dipósit de la Recerca de Catalunya
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,811543

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