Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption
- Autores
- Joshi, Reetika; Mandrini, Cristina Hemilse; Chandra, Ramesh; Schmieder, Brigitte; Cristiani, Germán Diego; Mac Cormack, Cecilia; Démoulin, Pascal; Cremades Fernandez, Maria Hebe
- Año de publicación
- 2022
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- How filaments form and erupt are topics about which solar researchers have wondered for more than a century and they are still open to debate. We present observations of a filament formation, its failed eruption, and the associated flare (SOL2019-05-09T05:51) that occurred in active region (AR) 12740 using data from the Solar Dynamics Observatory (SDO), the Solar-Terrestrial Relations Observatory A (STEREO-A), the Interface Region Imaging Spectrograph (IRIS) and the Learmonth Solar Observatory (LSO) of the National Solar Observatory/Global Oscillation Network Group (NSO/GONG). AR 12740 was a decaying region formed by a very disperse following polarity and a strong leading spot, surrounded by a highly dynamic zone where moving magnetic features (MMFs) were seen constantly diverging from the spot. Our analysis indicates that the filament was formed by the convergence of fibrils at a location where magnetic flux cancellation was observed. Furthermore, we conclude that its destabilisation was also related to flux cancellation associated with the constant shuffling of the MMFs. A two-ribbon flare occurred associated with the filament eruption; however, because the large-scale magnetic configuration of the AR was quadrupolar, two additional flare ribbons developed far from the two main ones. We model the magnetic configuration of the AR using a force-free field approach at the AR scale size. This local model is complemented by a global potential-field source-surface one. Based on the local model, we propose a scenario in which the filament failed eruption and the flare are due to two reconnection processes, one occurring below the erupting filament, leading to the two-ribbon flare, and another one above it between the filament flux-rope configuration and the large-scale closed loops. Our computation of the reconnected magnetic flux added to the erupting flux rope, compared to that of the large-scale field overlying it, allows us to conclude that the latter was large enough to prevent the filament eruption. A similar conjecture can be drawn from the computation of the magnetic tension derived from the global field model.
Fil: Joshi, Reetika. University of Oslo; Noruega
Fil: Mandrini, Cristina Hemilse. 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: Chandra, Ramesh. Kumaun University; India
Fil: Schmieder, Brigitte. Katholikie Universiteit Leuven; Bélgica. University of Glasgow; Reino Unido
Fil: Cristiani, Germán Diego. 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: Mac Cormack, Cecilia. 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: Démoulin, Pascal. Centre National de la Recherche Scientifique; Francia
Fil: Cremades Fernandez, Maria Hebe. Universidad de Mendoza. Facultad de Ingenieria; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza; Argentina - Materia
-
FLARES, DYNAMICS
HEATING, CORONAL
MAGNETIC FIELDS, CORONAL - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/197816
Ver los metadatos del registro completo
| id |
CONICETDig_705b267387994ce71590daa0ab2ae56b |
|---|---|
| oai_identifier_str |
oai:ri.conicet.gov.ar:11336/197816 |
| network_acronym_str |
CONICETDig |
| repository_id_str |
3498 |
| network_name_str |
CONICET Digital (CONICET) |
| spelling |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament EruptionJoshi, ReetikaMandrini, Cristina HemilseChandra, RameshSchmieder, BrigitteCristiani, Germán DiegoMac Cormack, CeciliaDémoulin, PascalCremades Fernandez, Maria HebeFLARES, DYNAMICSHEATING, CORONALMAGNETIC FIELDS, CORONALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1How filaments form and erupt are topics about which solar researchers have wondered for more than a century and they are still open to debate. We present observations of a filament formation, its failed eruption, and the associated flare (SOL2019-05-09T05:51) that occurred in active region (AR) 12740 using data from the Solar Dynamics Observatory (SDO), the Solar-Terrestrial Relations Observatory A (STEREO-A), the Interface Region Imaging Spectrograph (IRIS) and the Learmonth Solar Observatory (LSO) of the National Solar Observatory/Global Oscillation Network Group (NSO/GONG). AR 12740 was a decaying region formed by a very disperse following polarity and a strong leading spot, surrounded by a highly dynamic zone where moving magnetic features (MMFs) were seen constantly diverging from the spot. Our analysis indicates that the filament was formed by the convergence of fibrils at a location where magnetic flux cancellation was observed. Furthermore, we conclude that its destabilisation was also related to flux cancellation associated with the constant shuffling of the MMFs. A two-ribbon flare occurred associated with the filament eruption; however, because the large-scale magnetic configuration of the AR was quadrupolar, two additional flare ribbons developed far from the two main ones. We model the magnetic configuration of the AR using a force-free field approach at the AR scale size. This local model is complemented by a global potential-field source-surface one. Based on the local model, we propose a scenario in which the filament failed eruption and the flare are due to two reconnection processes, one occurring below the erupting filament, leading to the two-ribbon flare, and another one above it between the filament flux-rope configuration and the large-scale closed loops. Our computation of the reconnected magnetic flux added to the erupting flux rope, compared to that of the large-scale field overlying it, allows us to conclude that the latter was large enough to prevent the filament eruption. A similar conjecture can be drawn from the computation of the magnetic tension derived from the global field model.Fil: Joshi, Reetika. University of Oslo; NoruegaFil: Mandrini, Cristina Hemilse. 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: Chandra, Ramesh. Kumaun University; IndiaFil: Schmieder, Brigitte. Katholikie Universiteit Leuven; Bélgica. University of Glasgow; Reino UnidoFil: Cristiani, Germán Diego. 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: Mac Cormack, Cecilia. 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: Démoulin, Pascal. Centre National de la Recherche Scientifique; FranciaFil: Cremades Fernandez, Maria Hebe. Universidad de Mendoza. Facultad de Ingenieria; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza; ArgentinaSpringer2022-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/197816Joshi, Reetika; Mandrini, Cristina Hemilse; Chandra, Ramesh; Schmieder, Brigitte; Cristiani, Germán Diego; et al.; Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption; Springer; Solar Physics; 297; 7; 6-2022; 1-290038-0938CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-022-02021-5info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:21:23Zoai:ri.conicet.gov.ar:11336/197816instacron: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:34982025-10-22 11:21:24.165CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| title |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| spellingShingle |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption Joshi, Reetika FLARES, DYNAMICS HEATING, CORONAL MAGNETIC FIELDS, CORONAL |
| title_short |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| title_full |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| title_fullStr |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| title_full_unstemmed |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| title_sort |
Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption |
| dc.creator.none.fl_str_mv |
Joshi, Reetika Mandrini, Cristina Hemilse Chandra, Ramesh Schmieder, Brigitte Cristiani, Germán Diego Mac Cormack, Cecilia Démoulin, Pascal Cremades Fernandez, Maria Hebe |
| author |
Joshi, Reetika |
| author_facet |
Joshi, Reetika Mandrini, Cristina Hemilse Chandra, Ramesh Schmieder, Brigitte Cristiani, Germán Diego Mac Cormack, Cecilia Démoulin, Pascal Cremades Fernandez, Maria Hebe |
| author_role |
author |
| author2 |
Mandrini, Cristina Hemilse Chandra, Ramesh Schmieder, Brigitte Cristiani, Germán Diego Mac Cormack, Cecilia Démoulin, Pascal Cremades Fernandez, Maria Hebe |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
FLARES, DYNAMICS HEATING, CORONAL MAGNETIC FIELDS, CORONAL |
| topic |
FLARES, DYNAMICS HEATING, CORONAL MAGNETIC FIELDS, CORONAL |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
How filaments form and erupt are topics about which solar researchers have wondered for more than a century and they are still open to debate. We present observations of a filament formation, its failed eruption, and the associated flare (SOL2019-05-09T05:51) that occurred in active region (AR) 12740 using data from the Solar Dynamics Observatory (SDO), the Solar-Terrestrial Relations Observatory A (STEREO-A), the Interface Region Imaging Spectrograph (IRIS) and the Learmonth Solar Observatory (LSO) of the National Solar Observatory/Global Oscillation Network Group (NSO/GONG). AR 12740 was a decaying region formed by a very disperse following polarity and a strong leading spot, surrounded by a highly dynamic zone where moving magnetic features (MMFs) were seen constantly diverging from the spot. Our analysis indicates that the filament was formed by the convergence of fibrils at a location where magnetic flux cancellation was observed. Furthermore, we conclude that its destabilisation was also related to flux cancellation associated with the constant shuffling of the MMFs. A two-ribbon flare occurred associated with the filament eruption; however, because the large-scale magnetic configuration of the AR was quadrupolar, two additional flare ribbons developed far from the two main ones. We model the magnetic configuration of the AR using a force-free field approach at the AR scale size. This local model is complemented by a global potential-field source-surface one. Based on the local model, we propose a scenario in which the filament failed eruption and the flare are due to two reconnection processes, one occurring below the erupting filament, leading to the two-ribbon flare, and another one above it between the filament flux-rope configuration and the large-scale closed loops. Our computation of the reconnected magnetic flux added to the erupting flux rope, compared to that of the large-scale field overlying it, allows us to conclude that the latter was large enough to prevent the filament eruption. A similar conjecture can be drawn from the computation of the magnetic tension derived from the global field model. Fil: Joshi, Reetika. University of Oslo; Noruega Fil: Mandrini, Cristina Hemilse. 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: Chandra, Ramesh. Kumaun University; India Fil: Schmieder, Brigitte. Katholikie Universiteit Leuven; Bélgica. University of Glasgow; Reino Unido Fil: Cristiani, Germán Diego. 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: Mac Cormack, Cecilia. 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: Démoulin, Pascal. Centre National de la Recherche Scientifique; Francia Fil: Cremades Fernandez, Maria Hebe. Universidad de Mendoza. Facultad de Ingenieria; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Mendoza; Argentina |
| description |
How filaments form and erupt are topics about which solar researchers have wondered for more than a century and they are still open to debate. We present observations of a filament formation, its failed eruption, and the associated flare (SOL2019-05-09T05:51) that occurred in active region (AR) 12740 using data from the Solar Dynamics Observatory (SDO), the Solar-Terrestrial Relations Observatory A (STEREO-A), the Interface Region Imaging Spectrograph (IRIS) and the Learmonth Solar Observatory (LSO) of the National Solar Observatory/Global Oscillation Network Group (NSO/GONG). AR 12740 was a decaying region formed by a very disperse following polarity and a strong leading spot, surrounded by a highly dynamic zone where moving magnetic features (MMFs) were seen constantly diverging from the spot. Our analysis indicates that the filament was formed by the convergence of fibrils at a location where magnetic flux cancellation was observed. Furthermore, we conclude that its destabilisation was also related to flux cancellation associated with the constant shuffling of the MMFs. A two-ribbon flare occurred associated with the filament eruption; however, because the large-scale magnetic configuration of the AR was quadrupolar, two additional flare ribbons developed far from the two main ones. We model the magnetic configuration of the AR using a force-free field approach at the AR scale size. This local model is complemented by a global potential-field source-surface one. Based on the local model, we propose a scenario in which the filament failed eruption and the flare are due to two reconnection processes, one occurring below the erupting filament, leading to the two-ribbon flare, and another one above it between the filament flux-rope configuration and the large-scale closed loops. Our computation of the reconnected magnetic flux added to the erupting flux rope, compared to that of the large-scale field overlying it, allows us to conclude that the latter was large enough to prevent the filament eruption. A similar conjecture can be drawn from the computation of the magnetic tension derived from the global field model. |
| publishDate |
2022 |
| dc.date.none.fl_str_mv |
2022-06 |
| 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/11336/197816 Joshi, Reetika; Mandrini, Cristina Hemilse; Chandra, Ramesh; Schmieder, Brigitte; Cristiani, Germán Diego; et al.; Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption; Springer; Solar Physics; 297; 7; 6-2022; 1-29 0038-0938 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/197816 |
| identifier_str_mv |
Joshi, Reetika; Mandrini, Cristina Hemilse; Chandra, Ramesh; Schmieder, Brigitte; Cristiani, Germán Diego; et al.; Analysis of the Evolution of a Multi-Ribbon Flare and Failed Filament Eruption; Springer; Solar Physics; 297; 7; 6-2022; 1-29 0038-0938 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-022-02021-5 |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by/2.5/ar/ |
| eu_rights_str_mv |
openAccess |
| rights_invalid_str_mv |
https://creativecommons.org/licenses/by/2.5/ar/ |
| dc.format.none.fl_str_mv |
application/pdf application/pdf |
| dc.publisher.none.fl_str_mv |
Springer |
| publisher.none.fl_str_mv |
Springer |
| dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
| reponame_str |
CONICET Digital (CONICET) |
| collection |
CONICET Digital (CONICET) |
| instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
| _version_ |
1846781716294795264 |
| score |
12.982451 |