How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?

Autores
Mandrini, Cristina Hemilse; Nuevo, Federico Alberto; Vasquez, Alberto Marcos; Démoulin, Pascal; van Driel Gesztelyi, Lidia; Baker, D.; Culhane, J. l.; Cristiani, Germán Diego; Pick, M.
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Recent studies show that active-region (AR) upflowing plasma, ob- served by the EUV-Imaging Spectrometer (EIS), onboard Hinode, can gain access to open field-lines and be released into the solar wind (SW) via magnetic- interchange reconnection at magnetic null-points in pseudo-streamer configu- rations. When only one bipolar AR is present on the Sun and it is fully covered by the separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely that the upflowing AR plasma can find its way into the slow SW. However, signatures of plasma with AR composition have been found at 1 AU by Culhane et al. (2014) apparently originating from the West of AR 10978. We present a detailed topology analysis of AR 10978 and the surrounding large-scale corona based on a potential-field source-surface (PFSS) model. Our study shows that it is possible for the AR plasma to get around the streamer separatrix and be released into the SW via magnetic reconnection, occurring in at least two main steps. We analyse data from the Nan ̧cay Radioheliograph (NRH) searching for evidence of the chain of magnetic reconnections proposed. We find a noise storm above the AR and several varying sources at 150.9 MHz. Their locations suggest that they could be associated with particles accelerated during the first- step reconnection process and at a null point well outside of the AR. However, we find no evidence of the second-step reconnection in the radio data. Our results demonstrate that even when it appears highly improbable for the AR plasma to reach the SW, indirect channels involving a sequence of reconnections can make it possible.
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: Nuevo, Federico Alberto. 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: Vasquez, Alberto Marcos. 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: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Baker, D.. Ucl-mullard Space Science Laboratory; Reino Unido
Fil: Culhane, J. l.. Ucl-mullard Space Science Laboratory; Reino Unido
Fil: Cristiani, Germán Diego. 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: Pick, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Materia
Active Regions
Magnetic Fields
Magnetic Extrapolations
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:11336/17566
Acceder
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network_name_str CONICET Digital (CONICET)
spelling How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?Mandrini, Cristina HemilseNuevo, Federico AlbertoVasquez, Alberto MarcosDémoulin, Pascalvan Driel Gesztelyi, LidiaBaker, D.Culhane, J. l.Cristiani, Germán DiegoPick, M.Active RegionsMagnetic FieldsMagnetic Extrapolationshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Recent studies show that active-region (AR) upflowing plasma, ob- served by the EUV-Imaging Spectrometer (EIS), onboard Hinode, can gain access to open field-lines and be released into the solar wind (SW) via magnetic- interchange reconnection at magnetic null-points in pseudo-streamer configu- rations. When only one bipolar AR is present on the Sun and it is fully covered by the separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely that the upflowing AR plasma can find its way into the slow SW. However, signatures of plasma with AR composition have been found at 1 AU by Culhane et al. (2014) apparently originating from the West of AR 10978. We present a detailed topology analysis of AR 10978 and the surrounding large-scale corona based on a potential-field source-surface (PFSS) model. Our study shows that it is possible for the AR plasma to get around the streamer separatrix and be released into the SW via magnetic reconnection, occurring in at least two main steps. We analyse data from the Nan ̧cay Radioheliograph (NRH) searching for evidence of the chain of magnetic reconnections proposed. We find a noise storm above the AR and several varying sources at 150.9 MHz. Their locations suggest that they could be associated with particles accelerated during the first- step reconnection process and at a null point well outside of the AR. However, we find no evidence of the second-step reconnection in the radio data. Our results demonstrate that even when it appears highly improbable for the AR plasma to reach the SW, indirect channels involving a sequence of reconnections can make it possible.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; ArgentinaFil: Nuevo, Federico Alberto. 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: Vasquez, Alberto Marcos. 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: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Baker, D.. Ucl-mullard Space Science Laboratory; Reino UnidoFil: Culhane, J. l.. Ucl-mullard Space Science Laboratory; Reino UnidoFil: Cristiani, Germán Diego. 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: Pick, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaSpringer2014-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/17566Mandrini, Cristina Hemilse; Nuevo, Federico Alberto; Vasquez, Alberto Marcos; Démoulin, Pascal; van Driel Gesztelyi, Lidia; et al.; How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?; Springer; Solar Physics; 289; 11; 11-2014; 4151-41710038-0938enginfo:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-014-0582-yinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1409.7369info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-014-0582-yinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:15:59Zoai:ri.conicet.gov.ar:11336/17566instacron: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 10:15:59.628CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
title How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
spellingShingle How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
Mandrini, Cristina Hemilse
Active Regions
Magnetic Fields
Magnetic Extrapolations
title_short How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
title_full How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
title_fullStr How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
title_full_unstemmed How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
title_sort How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?
dc.creator.none.fl_str_mv Mandrini, Cristina Hemilse
Nuevo, Federico Alberto
Vasquez, Alberto Marcos
Démoulin, Pascal
van Driel Gesztelyi, Lidia
Baker, D.
Culhane, J. l.
Cristiani, Germán Diego
Pick, M.
author Mandrini, Cristina Hemilse
author_facet Mandrini, Cristina Hemilse
Nuevo, Federico Alberto
Vasquez, Alberto Marcos
Démoulin, Pascal
van Driel Gesztelyi, Lidia
Baker, D.
Culhane, J. l.
Cristiani, Germán Diego
Pick, M.
author_role author
author2 Nuevo, Federico Alberto
Vasquez, Alberto Marcos
Démoulin, Pascal
van Driel Gesztelyi, Lidia
Baker, D.
Culhane, J. l.
Cristiani, Germán Diego
Pick, M.
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Active Regions
Magnetic Fields
Magnetic Extrapolations
topic Active Regions
Magnetic Fields
Magnetic Extrapolations
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Recent studies show that active-region (AR) upflowing plasma, ob- served by the EUV-Imaging Spectrometer (EIS), onboard Hinode, can gain access to open field-lines and be released into the solar wind (SW) via magnetic- interchange reconnection at magnetic null-points in pseudo-streamer configu- rations. When only one bipolar AR is present on the Sun and it is fully covered by the separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely that the upflowing AR plasma can find its way into the slow SW. However, signatures of plasma with AR composition have been found at 1 AU by Culhane et al. (2014) apparently originating from the West of AR 10978. We present a detailed topology analysis of AR 10978 and the surrounding large-scale corona based on a potential-field source-surface (PFSS) model. Our study shows that it is possible for the AR plasma to get around the streamer separatrix and be released into the SW via magnetic reconnection, occurring in at least two main steps. We analyse data from the Nan ̧cay Radioheliograph (NRH) searching for evidence of the chain of magnetic reconnections proposed. We find a noise storm above the AR and several varying sources at 150.9 MHz. Their locations suggest that they could be associated with particles accelerated during the first- step reconnection process and at a null point well outside of the AR. However, we find no evidence of the second-step reconnection in the radio data. Our results demonstrate that even when it appears highly improbable for the AR plasma to reach the SW, indirect channels involving a sequence of reconnections can make it possible.
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: Nuevo, Federico Alberto. 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: Vasquez, Alberto Marcos. 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: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Baker, D.. Ucl-mullard Space Science Laboratory; Reino Unido
Fil: Culhane, J. l.. Ucl-mullard Space Science Laboratory; Reino Unido
Fil: Cristiani, Germán Diego. 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: Pick, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
description Recent studies show that active-region (AR) upflowing plasma, ob- served by the EUV-Imaging Spectrometer (EIS), onboard Hinode, can gain access to open field-lines and be released into the solar wind (SW) via magnetic- interchange reconnection at magnetic null-points in pseudo-streamer configu- rations. When only one bipolar AR is present on the Sun and it is fully covered by the separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely that the upflowing AR plasma can find its way into the slow SW. However, signatures of plasma with AR composition have been found at 1 AU by Culhane et al. (2014) apparently originating from the West of AR 10978. We present a detailed topology analysis of AR 10978 and the surrounding large-scale corona based on a potential-field source-surface (PFSS) model. Our study shows that it is possible for the AR plasma to get around the streamer separatrix and be released into the SW via magnetic reconnection, occurring in at least two main steps. We analyse data from the Nan ̧cay Radioheliograph (NRH) searching for evidence of the chain of magnetic reconnections proposed. We find a noise storm above the AR and several varying sources at 150.9 MHz. Their locations suggest that they could be associated with particles accelerated during the first- step reconnection process and at a null point well outside of the AR. However, we find no evidence of the second-step reconnection in the radio data. Our results demonstrate that even when it appears highly improbable for the AR plasma to reach the SW, indirect channels involving a sequence of reconnections can make it possible.
publishDate 2014
dc.date.none.fl_str_mv 2014-11
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/11336/17566
Mandrini, Cristina Hemilse; Nuevo, Federico Alberto; Vasquez, Alberto Marcos; Démoulin, Pascal; van Driel Gesztelyi, Lidia; et al.; How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?; Springer; Solar Physics; 289; 11; 11-2014; 4151-4171
0038-0938
url http://hdl.handle.net/11336/17566
identifier_str_mv Mandrini, Cristina Hemilse; Nuevo, Federico Alberto; Vasquez, Alberto Marcos; Démoulin, Pascal; van Driel Gesztelyi, Lidia; et al.; How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer?; Springer; Solar Physics; 289; 11; 11-2014; 4151-4171
0038-0938
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-014-0582-y
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1409.7369
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1007/s11207-014-0582-y
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
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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