Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA
- Autores
- Scolini, C.; Dasso, Sergio Ricardo; Rodriguez, L.; Zhukov, A. N.; Poedts, S.
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Coronal mass ejections (CMEs) are large-scale eruptions coming from the Sun and transiting into interplanetary space. While it is widely known that they are major drivers of space weather, further knowledge of CME properties in the inner heliosphere is limited by the scarcity of observations at heliocentric distances other than 1 au. In addition, most CMEs are observed in situ by a single spacecraft and in-depth studies require numerical models to complement the few available observations. Aims. We aim to assess the ability of the linear force-free spheromak CME model of the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) to describe the radial evolution of interplanetary CMEs in order to yield new contexts for observational studies. Methods. We modelled one well-studied CME with EUHFORIA, investigating its radial evolution by placing virtual spacecraft along the Sun-Earth line in the simulation domain. To directly compare observational and modelling results, we characterised the interplanetary CME signatures between 0.2 and 1.9 au from modelled time series, exploiting techniques that are traditionally employed to analyse real in situ data. Results. Our results show that the modelled radial evolution of the mean solar wind and CME values is consistent with the observational and theoretical expectations. The CME expands as a consequence of the decaying pressure in the surrounding solar wind: the expansion is rapid within 0.4 au and moderate at larger distances. The early rapid expansion was not sufficient to explain the overestimated CME radial size in our simulation, suggesting this is an intrinsic limitation of the spheromak geometry applied in this case. The magnetic field profile indicates a relaxation on the part of the CME structure during propagation, while CME ageing is most probably not a substantial source of magnetic asymmetry beyond 0.4 au. Finally, we report a CME wake that is significantly shorter than what has been suggested by observations. Conclusions. Overall, EUHFORIA provides a consistent description of the radial evolution of solar wind and CMEs, at least close to their centres. Nevertheless, improvements are required to better reproduce the CME radial extension.
Fil: Scolini, C.. Royal Observatory of Belgium; Bélgica
Fil: Dasso, Sergio Ricardo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Rodriguez, L.. Observatorio Pierre Auger; Argentina
Fil: Zhukov, A. N.. Observatorio Pierre Auger; Argentina
Fil: Poedts, S.. Observatorio Pierre Auger; Argentina - Materia
-
MAGNETOHYDRODYNAMICS (MHD)
SOLAR WIND
SUN: CORONAL MASS EJECTIONS (CMES)
SUN: HELIOSPHERE - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/182214
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CONICET Digital (CONICET) |
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Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIAScolini, C.Dasso, Sergio RicardoRodriguez, L.Zhukov, A. N.Poedts, S.MAGNETOHYDRODYNAMICS (MHD)SOLAR WINDSUN: CORONAL MASS EJECTIONS (CMES)SUN: HELIOSPHEREhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Coronal mass ejections (CMEs) are large-scale eruptions coming from the Sun and transiting into interplanetary space. While it is widely known that they are major drivers of space weather, further knowledge of CME properties in the inner heliosphere is limited by the scarcity of observations at heliocentric distances other than 1 au. In addition, most CMEs are observed in situ by a single spacecraft and in-depth studies require numerical models to complement the few available observations. Aims. We aim to assess the ability of the linear force-free spheromak CME model of the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) to describe the radial evolution of interplanetary CMEs in order to yield new contexts for observational studies. Methods. We modelled one well-studied CME with EUHFORIA, investigating its radial evolution by placing virtual spacecraft along the Sun-Earth line in the simulation domain. To directly compare observational and modelling results, we characterised the interplanetary CME signatures between 0.2 and 1.9 au from modelled time series, exploiting techniques that are traditionally employed to analyse real in situ data. Results. Our results show that the modelled radial evolution of the mean solar wind and CME values is consistent with the observational and theoretical expectations. The CME expands as a consequence of the decaying pressure in the surrounding solar wind: the expansion is rapid within 0.4 au and moderate at larger distances. The early rapid expansion was not sufficient to explain the overestimated CME radial size in our simulation, suggesting this is an intrinsic limitation of the spheromak geometry applied in this case. The magnetic field profile indicates a relaxation on the part of the CME structure during propagation, while CME ageing is most probably not a substantial source of magnetic asymmetry beyond 0.4 au. Finally, we report a CME wake that is significantly shorter than what has been suggested by observations. Conclusions. Overall, EUHFORIA provides a consistent description of the radial evolution of solar wind and CMEs, at least close to their centres. Nevertheless, improvements are required to better reproduce the CME radial extension.Fil: Scolini, C.. Royal Observatory of Belgium; BélgicaFil: Dasso, Sergio Ricardo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Rodriguez, L.. Observatorio Pierre Auger; ArgentinaFil: Zhukov, A. N.. Observatorio Pierre Auger; ArgentinaFil: Poedts, S.. Observatorio Pierre Auger; ArgentinaEDP Sciences2021-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/182214Scolini, C.; Dasso, Sergio Ricardo; Rodriguez, L.; Zhukov, A. N.; Poedts, S.; Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-200004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202040226info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202040226info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:25:48Zoai:ri.conicet.gov.ar:11336/182214instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:25:48.328CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
title |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
spellingShingle |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA Scolini, C. MAGNETOHYDRODYNAMICS (MHD) SOLAR WIND SUN: CORONAL MASS EJECTIONS (CMES) SUN: HELIOSPHERE |
title_short |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
title_full |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
title_fullStr |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
title_full_unstemmed |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
title_sort |
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA |
dc.creator.none.fl_str_mv |
Scolini, C. Dasso, Sergio Ricardo Rodriguez, L. Zhukov, A. N. Poedts, S. |
author |
Scolini, C. |
author_facet |
Scolini, C. Dasso, Sergio Ricardo Rodriguez, L. Zhukov, A. N. Poedts, S. |
author_role |
author |
author2 |
Dasso, Sergio Ricardo Rodriguez, L. Zhukov, A. N. Poedts, S. |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
MAGNETOHYDRODYNAMICS (MHD) SOLAR WIND SUN: CORONAL MASS EJECTIONS (CMES) SUN: HELIOSPHERE |
topic |
MAGNETOHYDRODYNAMICS (MHD) SOLAR WIND SUN: CORONAL MASS EJECTIONS (CMES) SUN: HELIOSPHERE |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Context. Coronal mass ejections (CMEs) are large-scale eruptions coming from the Sun and transiting into interplanetary space. While it is widely known that they are major drivers of space weather, further knowledge of CME properties in the inner heliosphere is limited by the scarcity of observations at heliocentric distances other than 1 au. In addition, most CMEs are observed in situ by a single spacecraft and in-depth studies require numerical models to complement the few available observations. Aims. We aim to assess the ability of the linear force-free spheromak CME model of the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) to describe the radial evolution of interplanetary CMEs in order to yield new contexts for observational studies. Methods. We modelled one well-studied CME with EUHFORIA, investigating its radial evolution by placing virtual spacecraft along the Sun-Earth line in the simulation domain. To directly compare observational and modelling results, we characterised the interplanetary CME signatures between 0.2 and 1.9 au from modelled time series, exploiting techniques that are traditionally employed to analyse real in situ data. Results. Our results show that the modelled radial evolution of the mean solar wind and CME values is consistent with the observational and theoretical expectations. The CME expands as a consequence of the decaying pressure in the surrounding solar wind: the expansion is rapid within 0.4 au and moderate at larger distances. The early rapid expansion was not sufficient to explain the overestimated CME radial size in our simulation, suggesting this is an intrinsic limitation of the spheromak geometry applied in this case. The magnetic field profile indicates a relaxation on the part of the CME structure during propagation, while CME ageing is most probably not a substantial source of magnetic asymmetry beyond 0.4 au. Finally, we report a CME wake that is significantly shorter than what has been suggested by observations. Conclusions. Overall, EUHFORIA provides a consistent description of the radial evolution of solar wind and CMEs, at least close to their centres. Nevertheless, improvements are required to better reproduce the CME radial extension. Fil: Scolini, C.. Royal Observatory of Belgium; Bélgica Fil: Dasso, Sergio Ricardo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Rodriguez, L.. Observatorio Pierre Auger; Argentina Fil: Zhukov, A. N.. Observatorio Pierre Auger; Argentina Fil: Poedts, S.. Observatorio Pierre Auger; Argentina |
description |
Context. Coronal mass ejections (CMEs) are large-scale eruptions coming from the Sun and transiting into interplanetary space. While it is widely known that they are major drivers of space weather, further knowledge of CME properties in the inner heliosphere is limited by the scarcity of observations at heliocentric distances other than 1 au. In addition, most CMEs are observed in situ by a single spacecraft and in-depth studies require numerical models to complement the few available observations. Aims. We aim to assess the ability of the linear force-free spheromak CME model of the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) to describe the radial evolution of interplanetary CMEs in order to yield new contexts for observational studies. Methods. We modelled one well-studied CME with EUHFORIA, investigating its radial evolution by placing virtual spacecraft along the Sun-Earth line in the simulation domain. To directly compare observational and modelling results, we characterised the interplanetary CME signatures between 0.2 and 1.9 au from modelled time series, exploiting techniques that are traditionally employed to analyse real in situ data. Results. Our results show that the modelled radial evolution of the mean solar wind and CME values is consistent with the observational and theoretical expectations. The CME expands as a consequence of the decaying pressure in the surrounding solar wind: the expansion is rapid within 0.4 au and moderate at larger distances. The early rapid expansion was not sufficient to explain the overestimated CME radial size in our simulation, suggesting this is an intrinsic limitation of the spheromak geometry applied in this case. The magnetic field profile indicates a relaxation on the part of the CME structure during propagation, while CME ageing is most probably not a substantial source of magnetic asymmetry beyond 0.4 au. Finally, we report a CME wake that is significantly shorter than what has been suggested by observations. Conclusions. Overall, EUHFORIA provides a consistent description of the radial evolution of solar wind and CMEs, at least close to their centres. Nevertheless, improvements are required to better reproduce the CME radial extension. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-05 |
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/11336/182214 Scolini, C.; Dasso, Sergio Ricardo; Rodriguez, L.; Zhukov, A. N.; Poedts, S.; Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-20 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/182214 |
identifier_str_mv |
Scolini, C.; Dasso, Sergio Ricardo; Rodriguez, L.; Zhukov, A. N.; Poedts, S.; Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-20 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202040226 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202040226 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
EDP Sciences |
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EDP Sciences |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1844614257589616640 |
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13.070432 |