On the partial eruption of a bifurcated solar filament structure

The partial eruption of a filament channel with bifurcated substructures is investigated using data sets obtained from both ground-based and space-borne facilities. Small-scale flux reconnection/cancellation events in the region triggered the pile-up of ambient magnetic field, observed as bright ext...

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Autores: Monga, Aabha, Sharma, Rahul, Liu, Jiajia, Cid Tortuero, Consuelo|||0000-0002-2863-3745, Uddin, Wahab, Chandra, Ramesh, Erdélyi, Robertus
Tipo de recurso: artículo
Fecha de publicación:2021
País:España
Institución:Universidad de Alcalá (UAH)
Repositorio:e_Buah Biblioteca Digital Universidad de Alcalá
Idioma:inglés
OAI Identifier:oai:ebuah.uah.es:10017/67679
Acceso en línea:http://hdl.handle.net/10017/67679
https://dx.doi.org/10.1093/mnras/staa2902
Access Level:acceso abierto
Palabra clave:Sun: coronal mass ejections (CMEs)
Sun: filaments, prominences
Sun: flares
Sun: magnetic fields
Astronomía
Astronomy
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spelling On the partial eruption of a bifurcated solar filament structureMonga, AabhaSharma, RahulLiu, JiajiaCid Tortuero, Consuelo|||0000-0002-2863-3745Uddin, WahabChandra, RameshErdélyi, RobertusSun: coronal mass ejections (CMEs)Sun: filaments, prominencesSun: flaresSun: magnetic fieldsAstronomíaAstronomyThe partial eruption of a filament channel with bifurcated substructures is investigated using data sets obtained from both ground-based and space-borne facilities. Small-scale flux reconnection/cancellation events in the region triggered the pile-up of ambient magnetic field, observed as bright extreme ultraviolet (EUV) loops in close proximity to the filament channel. This led to the formation of a V-shaped cusp structure at the site of interaction between the coalesced EUV loops and the filament channel, with the presence of distinct plasmoid structures and associated bidirectional flows. Analysis of imaging data from SDO/AIA further suggests vertical splitting of the filament structure into two substructures. The perturbed upper branch of the filament structure rose up and erupted with the onset of an energetic GOES M1.4 flare at 04:30 UT on 2015 January 28. The estimated twist number and squashing factor obtained from non-linear force free-field extrapolation of the magnetic field data support the vertical split in the filament structure with high twist in the upper substructure. The loss in equilibrium of the upper branch due to torus instability implies that this is a potential triggering mechanism for the observed partial eruption.Oxford Academic20212021-01-01journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10017/67679https://dx.doi.org/10.1093/mnras/staa2902reponame:e_Buah Biblioteca Digital Universidad de Alcaláinstname:Universidad de Alcalá (UAH)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Attribution-NonCommercial-NoDerivatives 4.0 Internationalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:ebuah.uah.es:10017/676792026-06-18T11:13:07Z
dc.title.none.fl_str_mv On the partial eruption of a bifurcated solar filament structure
title On the partial eruption of a bifurcated solar filament structure
spellingShingle On the partial eruption of a bifurcated solar filament structure
Monga, Aabha
Sun: coronal mass ejections (CMEs)
Sun: filaments, prominences
Sun: flares
Sun: magnetic fields
Astronomía
Astronomy
title_short On the partial eruption of a bifurcated solar filament structure
title_full On the partial eruption of a bifurcated solar filament structure
title_fullStr On the partial eruption of a bifurcated solar filament structure
title_full_unstemmed On the partial eruption of a bifurcated solar filament structure
title_sort On the partial eruption of a bifurcated solar filament structure
dc.creator.none.fl_str_mv Monga, Aabha
Sharma, Rahul
Liu, Jiajia
Cid Tortuero, Consuelo|||0000-0002-2863-3745
Uddin, Wahab
Chandra, Ramesh
Erdélyi, Robertus
author Monga, Aabha
author_facet Monga, Aabha
Sharma, Rahul
Liu, Jiajia
Cid Tortuero, Consuelo|||0000-0002-2863-3745
Uddin, Wahab
Chandra, Ramesh
Erdélyi, Robertus
author_role author
author2 Sharma, Rahul
Liu, Jiajia
Cid Tortuero, Consuelo|||0000-0002-2863-3745
Uddin, Wahab
Chandra, Ramesh
Erdélyi, Robertus
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Sun: coronal mass ejections (CMEs)
Sun: filaments, prominences
Sun: flares
Sun: magnetic fields
Astronomía
Astronomy
topic Sun: coronal mass ejections (CMEs)
Sun: filaments, prominences
Sun: flares
Sun: magnetic fields
Astronomía
Astronomy
description The partial eruption of a filament channel with bifurcated substructures is investigated using data sets obtained from both ground-based and space-borne facilities. Small-scale flux reconnection/cancellation events in the region triggered the pile-up of ambient magnetic field, observed as bright extreme ultraviolet (EUV) loops in close proximity to the filament channel. This led to the formation of a V-shaped cusp structure at the site of interaction between the coalesced EUV loops and the filament channel, with the presence of distinct plasmoid structures and associated bidirectional flows. Analysis of imaging data from SDO/AIA further suggests vertical splitting of the filament structure into two substructures. The perturbed upper branch of the filament structure rose up and erupted with the onset of an energetic GOES M1.4 flare at 04:30 UT on 2015 January 28. The estimated twist number and squashing factor obtained from non-linear force free-field extrapolation of the magnetic field data support the vertical split in the filament structure with high twist in the upper substructure. The loss in equilibrium of the upper branch due to torus instability implies that this is a potential triggering mechanism for the observed partial eruption.
publishDate 2021
dc.date.none.fl_str_mv 2021
2021-01-01
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/10017/67679
https://dx.doi.org/10.1093/mnras/staa2902
url http://hdl.handle.net/10017/67679
https://dx.doi.org/10.1093/mnras/staa2902
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-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/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-NonCommercial-NoDerivatives 4.0 International
http://creativecommons.org/licenses/by-nc-nd/4.0/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Oxford Academic
publisher.none.fl_str_mv Oxford Academic
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 15,812429

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