Filament interaction modeled by flux rope reconnection

Autores
Török, T.; Chandra, R.; Pariat, E.; Démoulin, Pascal; Schmieder, B.; Aulanier, G.; Linton, M.; Mandrini, Cristina Hemilse
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of “slingshot” reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Demoulin as the initial condition for the magnetic field. To this end, a ´ configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments.
Fil: Török, T.. Université Paris Diderot - Paris 7; Francia
Fil: Chandra, R.. Université Paris Diderot - Paris 7; Francia
Fil: Pariat, E.. Université Paris Diderot - Paris 7; Francia
Fil: Démoulin, Pascal. Université Paris Diderot - Paris 7; Francia
Fil: Schmieder, B.. Université Paris Diderot - Paris 7; Francia
Fil: Aulanier, G.. Université Paris Diderot - Paris 7; Francia
Fil: Linton, M.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
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
Materia
Sun - Corona
Sun - Prominences -Filaments
Numerical Methods
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:11336/19621
Acceder
id CONICETDig_9c9e5778c14f47debfd121ba95b6e6af
oai_identifier_str oai:ri.conicet.gov.ar:11336/19621
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Filament interaction modeled by flux rope reconnectionTörök, T.Chandra, R.Pariat, E.Démoulin, PascalSchmieder, B.Aulanier, G.Linton, M.Mandrini, Cristina HemilseSun - CoronaSun - Prominences -FilamentsNumerical Methodshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of “slingshot” reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Demoulin as the initial condition for the magnetic field. To this end, a ´ configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments.Fil: Török, T.. Université Paris Diderot - Paris 7; FranciaFil: Chandra, R.. Université Paris Diderot - Paris 7; FranciaFil: Pariat, E.. Université Paris Diderot - Paris 7; FranciaFil: Démoulin, Pascal. Université Paris Diderot - Paris 7; FranciaFil: Schmieder, B.. Université Paris Diderot - Paris 7; FranciaFil: Aulanier, G.. Université Paris Diderot - Paris 7; FranciaFil: Linton, M.. Spece Sciences División. Naval Research Laboratory; Estados UnidosFil: 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; ArgentinaIOP Publishing2011-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19621Török, T.; Chandra, R.; Pariat, E.; Démoulin, Pascal; Schmieder, B.; et al.; Filament interaction modeled by flux rope reconnection; IOP Publishing; Astrophysical Journal; 728; 1; 2-2011; 1-6; 650004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/728/1/65info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/728/1/65/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:46:50Zoai:ri.conicet.gov.ar:11336/19621instacron: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 11:46:50.693CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Filament interaction modeled by flux rope reconnection
title Filament interaction modeled by flux rope reconnection
spellingShingle Filament interaction modeled by flux rope reconnection
Török, T.
Sun - Corona
Sun - Prominences -Filaments
Numerical Methods
title_short Filament interaction modeled by flux rope reconnection
title_full Filament interaction modeled by flux rope reconnection
title_fullStr Filament interaction modeled by flux rope reconnection
title_full_unstemmed Filament interaction modeled by flux rope reconnection
title_sort Filament interaction modeled by flux rope reconnection
dc.creator.none.fl_str_mv Török, T.
Chandra, R.
Pariat, E.
Démoulin, Pascal
Schmieder, B.
Aulanier, G.
Linton, M.
Mandrini, Cristina Hemilse
author Török, T.
author_facet Török, T.
Chandra, R.
Pariat, E.
Démoulin, Pascal
Schmieder, B.
Aulanier, G.
Linton, M.
Mandrini, Cristina Hemilse
author_role author
author2 Chandra, R.
Pariat, E.
Démoulin, Pascal
Schmieder, B.
Aulanier, G.
Linton, M.
Mandrini, Cristina Hemilse
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Sun - Corona
Sun - Prominences -Filaments
Numerical Methods
topic Sun - Corona
Sun - Prominences -Filaments
Numerical Methods
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of “slingshot” reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Demoulin as the initial condition for the magnetic field. To this end, a ´ configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments.
Fil: Török, T.. Université Paris Diderot - Paris 7; Francia
Fil: Chandra, R.. Université Paris Diderot - Paris 7; Francia
Fil: Pariat, E.. Université Paris Diderot - Paris 7; Francia
Fil: Démoulin, Pascal. Université Paris Diderot - Paris 7; Francia
Fil: Schmieder, B.. Université Paris Diderot - Paris 7; Francia
Fil: Aulanier, G.. Université Paris Diderot - Paris 7; Francia
Fil: Linton, M.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
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
description Hα observations of solar active region NOAA 10501 on 2003 November 20 revealed a very uncommon dynamic process: during the development of a nearby flare, two adjacent elongated filaments approached each other, merged at their middle sections, and separated again, thereby forming stable configurations with new footpoint connections. The observed dynamic pattern is indicative of “slingshot” reconnection between two magnetic flux ropes. We test this scenario by means of a three-dimensional zero β magnetohydrodynamic simulation, using a modified version of the coronal flux rope model by Titov and Demoulin as the initial condition for the magnetic field. To this end, a ´ configuration is constructed that contains two flux ropes which are oriented side-by-side and are embedded in an ambient potential field. The choice of the magnetic orientation of the flux ropes and of the topology of the potential field is guided by the observations. Quasi-static boundary flows are then imposed to bring the middle sections of the flux ropes into contact. After sufficient driving, the ropes reconnect and two new flux ropes are formed, which now connect the former adjacent flux rope footpoints of opposite polarity. The corresponding evolution of filament material is modeled by calculating the positions of field line dips at all times. The dips follow the morphological evolution of the flux ropes, in qualitative agreement with the observed filaments.
publishDate 2011
dc.date.none.fl_str_mv 2011-02
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/11336/19621
Török, T.; Chandra, R.; Pariat, E.; Démoulin, Pascal; Schmieder, B.; et al.; Filament interaction modeled by flux rope reconnection; IOP Publishing; Astrophysical Journal; 728; 1; 2-2011; 1-6; 65
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/19621
identifier_str_mv Török, T.; Chandra, R.; Pariat, E.; Démoulin, Pascal; Schmieder, B.; et al.; Filament interaction modeled by flux rope reconnection; IOP Publishing; Astrophysical Journal; 728; 1; 2-2011; 1-6; 65
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/728/1/65
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/728/1/65/meta
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 IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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_ 1846782171540357120
score 12.982451

Publicaciones similares