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dc.contributor.author
Scolini, C.
dc.contributor.author
Dasso, Sergio Ricardo
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Rodriguez, L.
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Zhukov, A. N.
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Poedts, S.
dc.date.available
2022-12-22T15:55:27Z
dc.date.issued
2021-05
dc.identifier.citation
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
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/182214
dc.description.abstract
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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
MAGNETOHYDRODYNAMICS (MHD)
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SOLAR WIND
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SUN: CORONAL MASS EJECTIONS (CMES)
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SUN: HELIOSPHERE
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
Exploring the radial evolution of interplanetary coronal mass ejections using EUHFORIA
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2022-09-23T10:13:31Z
dc.journal.volume
649
dc.journal.pagination
1-20
dc.journal.pais
Francia
dc.journal.ciudad
Paris
dc.description.fil
Fil: Scolini, C.. Royal Observatory of Belgium; Bélgica
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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
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Fil: Rodriguez, L.. Observatorio Pierre Auger; Argentina
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Fil: Zhukov, A. N.. Observatorio Pierre Auger; Argentina
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Fil: Poedts, S.. Observatorio Pierre Auger; Argentina
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202040226
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/202040226
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