Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003

Autores
Chandra, R.; Schmieder, B.; Mandrini, Cristina Hemilse; Démoulin, Pascal; Pariat, E.; Torok, T.; Uddin, W.
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both events
Fil: Chandra, R.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes 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. Observatoire de Paris; Francia
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Torok, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Uddin, W.. Aryabhatta Research Institute of Observational Sciences; India
Materia
Active Regions
Magnetic Field
Flare Dynamics
Flares - Relation to Magnetic Field
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/19625
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/19625
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003Chandra, R.Schmieder, B.Mandrini, Cristina HemilseDémoulin, PascalPariat, E.Torok, T.Uddin, W.Active RegionsMagnetic FieldFlare DynamicsFlares - Relation to Magnetic Fieldhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both eventsFil: Chandra, R.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes 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. Observatoire de Paris; FranciaFil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Torok, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Uddin, W.. Aryabhatta Research Institute of Observational Sciences; IndiaSpringer2011-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19625Chandra, R.; Schmieder, B.; Mandrini, Cristina Hemilse; Démoulin, Pascal; Pariat, E.; et al.; Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003; Springer; Solar Physics; 269; 1; 3-2011; 83-1040038-0938CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-010-9670-9info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1011.1187info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-010-9670-9info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:35:47Zoai:ri.conicet.gov.ar:11336/19625instacron: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 09:35:48.223CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
title Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
spellingShingle Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
Chandra, R.
Active Regions
Magnetic Field
Flare Dynamics
Flares - Relation to Magnetic Field
title_short Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
title_full Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
title_fullStr Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
title_full_unstemmed Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
title_sort Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003
dc.creator.none.fl_str_mv Chandra, R.
Schmieder, B.
Mandrini, Cristina Hemilse
Démoulin, Pascal
Pariat, E.
Torok, T.
Uddin, W.
author Chandra, R.
author_facet Chandra, R.
Schmieder, B.
Mandrini, Cristina Hemilse
Démoulin, Pascal
Pariat, E.
Torok, T.
Uddin, W.
author_role author
author2 Schmieder, B.
Mandrini, Cristina Hemilse
Démoulin, Pascal
Pariat, E.
Torok, T.
Uddin, W.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv Active Regions
Magnetic Field
Flare Dynamics
Flares - Relation to Magnetic Field
topic Active Regions
Magnetic Field
Flare Dynamics
Flares - Relation to Magnetic Field
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both events
Fil: Chandra, R.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes 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. Observatoire de Paris; Francia
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Torok, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Uddin, W.. Aryabhatta Research Institute of Observational Sciences; India
description We present and interpret observations of two morphologically homologous flares that occurred in active region (AR) NOAA 10501 on 20 November 2003. Both flares displayed four homologous Hα ribbons and were both accompanied by coronal mass ejections (CMEs). The central flare ribbons were located at the site of an emerging bipole in the centre of the active region. The negative polarity of this bipole fragmented in two main pieces, one rotating around the positive polarity by ≈110° within 32 hours. We model the coronal magnetic field and compute its topology, using as boundary condition the magnetogram closest in time to each flare. In particular, we calculate the location of quasi-separatrix layers (QSLs) in order to understand the connectivity between the flare ribbons. Though several polarities were present in AR 10501, the global magnetic field topology corresponds to a quadrupolar magnetic field distribution without magnetic null points. For both flares, the photospheric traces of QSLs are similar and match well the locations of the four Hα ribbons. This globally unchanged topology and the continuous shearing by the rotating bipole are two key factors responsible for the flare homology. However, our analyses also indicate that different magnetic connectivity domains of the quadrupolar configuration become unstable during each flare, so that magnetic reconnection proceeds differently in both events
publishDate 2011
dc.date.none.fl_str_mv 2011-03
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/11336/19625
Chandra, R.; Schmieder, B.; Mandrini, Cristina Hemilse; Démoulin, Pascal; Pariat, E.; et al.; Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003; Springer; Solar Physics; 269; 1; 3-2011; 83-104
0038-0938
CONICET Digital
CONICET
url http://hdl.handle.net/11336/19625
identifier_str_mv Chandra, R.; Schmieder, B.; Mandrini, Cristina Hemilse; Démoulin, Pascal; Pariat, E.; et al.; Homologous flares and magnetic field topology in active region NOAA 10501 on 20 November 2003; Springer; Solar Physics; 269; 1; 3-2011; 83-104
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/s11207-010-9670-9
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1011.1187
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-010-9670-9
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
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
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score 13.070432

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