Blowouts jets and impulsive eruptive flares in a bald-patch topology
- Autores
- Chandra, R.; Mandrini, Cristina Hemilse; Schmieder, B.; Joshi, B.; Cristiani, Germán Diego; Cremades Fernandez, Maria Hebe; Pariat, E.; Nuevo, Federico Alberto; Srivastava, A. K.; Uddi, W.
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. A subclass of broad extreme ultraviolet (EUV) and X-ray jets, called blowout jets, have become a topic of research since they could be the link between standard collimated jets and coronal mass ejections (CMEs). Aims. Our aim is to understand the origin of a series of broad jets, some of which are accompanied by flares and associated with narrow and jet-like CMEs. Methods. We analyze observations of a series of recurrent broad jets observed in AR 10484 on 21?24 October 2003. In particular, one of them occurred simultaneously with an M2.4 flare on 23 October at 02:41 UT (SOLA2003-10-23). Both events were observed by the ARIES Hα Solar Tower-Telescope, TRACE, SOHO, and RHESSI instruments. The flare was very impulsive and followed by a narrow CME. A local force-free model of AR 10484 is the basis to compute its topology. We find bald patches (BPs) at the flare site. This BP topology is present for at least two days before to events. Large-scale field lines, associated with the BPs, represent open loops. This is confirmed by a global potential free source surface (PFSS) model. Following the brightest leading edge of the Hα and EUV jet emission, we can temporarily associate these emissions with a narrow CME. Results. Considering their characteristics, the observed broad jets appear to be of the blowout class. As the most plausible scenario, we propose that magnetic reconnection could occur at the BP separatrices forced by the destabilization of a continuously reformed flux rope underlying them. The reconnection process could bring the cool flux-rope material into the reconnected open field lines driving the series of recurrent blowout jets and accompanying CMEs. Conclusions. Based on a model of the coronal field, we compute the AR 10484 topology at the location where flaring and blowout jets occurred from 21 to 24 October 2003. This topology can consistently explain the origin of these events.
Fil: Chandra, R.. Kumaun University; India
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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Joshi, B.. Udaipur Solar Observatory; India
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: Cremades Fernandez, Maria Hebe. Universidad Tecnologica Nacional; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
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: Srivastava, A. K.. Indian Institute Of Technology; India
Fil: Uddi, W.. Aryabhatta Research Institute of Observational Sciences; India - Materia
- Sun: magnetic field
- Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/21704
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oai:ri.conicet.gov.ar:11336/21704 |
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CONICET Digital (CONICET) |
spelling |
Blowouts jets and impulsive eruptive flares in a bald-patch topologyChandra, R.Mandrini, Cristina HemilseSchmieder, B.Joshi, B.Cristiani, Germán DiegoCremades Fernandez, Maria HebePariat, E.Nuevo, Federico AlbertoSrivastava, A. K.Uddi, W.Sun: magnetic fieldhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. A subclass of broad extreme ultraviolet (EUV) and X-ray jets, called blowout jets, have become a topic of research since they could be the link between standard collimated jets and coronal mass ejections (CMEs). Aims. Our aim is to understand the origin of a series of broad jets, some of which are accompanied by flares and associated with narrow and jet-like CMEs. Methods. We analyze observations of a series of recurrent broad jets observed in AR 10484 on 21?24 October 2003. In particular, one of them occurred simultaneously with an M2.4 flare on 23 October at 02:41 UT (SOLA2003-10-23). Both events were observed by the ARIES Hα Solar Tower-Telescope, TRACE, SOHO, and RHESSI instruments. The flare was very impulsive and followed by a narrow CME. A local force-free model of AR 10484 is the basis to compute its topology. We find bald patches (BPs) at the flare site. This BP topology is present for at least two days before to events. Large-scale field lines, associated with the BPs, represent open loops. This is confirmed by a global potential free source surface (PFSS) model. Following the brightest leading edge of the Hα and EUV jet emission, we can temporarily associate these emissions with a narrow CME. Results. Considering their characteristics, the observed broad jets appear to be of the blowout class. As the most plausible scenario, we propose that magnetic reconnection could occur at the BP separatrices forced by the destabilization of a continuously reformed flux rope underlying them. The reconnection process could bring the cool flux-rope material into the reconnected open field lines driving the series of recurrent blowout jets and accompanying CMEs. Conclusions. Based on a model of the coronal field, we compute the AR 10484 topology at the location where flaring and blowout jets occurred from 21 to 24 October 2003. This topology can consistently explain the origin of these events.Fil: Chandra, R.. Kumaun University; IndiaFil: 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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Joshi, B.. Udaipur Solar Observatory; IndiaFil: 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: Cremades Fernandez, Maria Hebe. Universidad Tecnologica Nacional; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: 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: Srivastava, A. K.. Indian Institute Of Technology; IndiaFil: Uddi, W.. Aryabhatta Research Institute of Observational Sciences; IndiaEDP Sciences2017-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21704Chandra, R.; Mandrini, Cristina Hemilse; Schmieder, B.; Joshi, B.; Cristiani, Germán Diego; et al.; Blowouts jets and impulsive eruptive flares in a bald-patch topology; EDP Sciences; Astronomy and Astrophysics; 598; A41; 1-2017; 1-150004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2017/02/aa28984-16/aa28984-16.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628984info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:46:23Zoai:ri.conicet.gov.ar:11336/21704instacron: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 10:46:24.062CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
title |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
spellingShingle |
Blowouts jets and impulsive eruptive flares in a bald-patch topology Chandra, R. Sun: magnetic field |
title_short |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
title_full |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
title_fullStr |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
title_full_unstemmed |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
title_sort |
Blowouts jets and impulsive eruptive flares in a bald-patch topology |
dc.creator.none.fl_str_mv |
Chandra, R. Mandrini, Cristina Hemilse Schmieder, B. Joshi, B. Cristiani, Germán Diego Cremades Fernandez, Maria Hebe Pariat, E. Nuevo, Federico Alberto Srivastava, A. K. Uddi, W. |
author |
Chandra, R. |
author_facet |
Chandra, R. Mandrini, Cristina Hemilse Schmieder, B. Joshi, B. Cristiani, Germán Diego Cremades Fernandez, Maria Hebe Pariat, E. Nuevo, Federico Alberto Srivastava, A. K. Uddi, W. |
author_role |
author |
author2 |
Mandrini, Cristina Hemilse Schmieder, B. Joshi, B. Cristiani, Germán Diego Cremades Fernandez, Maria Hebe Pariat, E. Nuevo, Federico Alberto Srivastava, A. K. Uddi, W. |
author2_role |
author author author author author author author author author |
dc.subject.none.fl_str_mv |
Sun: magnetic field |
topic |
Sun: 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 |
Context. A subclass of broad extreme ultraviolet (EUV) and X-ray jets, called blowout jets, have become a topic of research since they could be the link between standard collimated jets and coronal mass ejections (CMEs). Aims. Our aim is to understand the origin of a series of broad jets, some of which are accompanied by flares and associated with narrow and jet-like CMEs. Methods. We analyze observations of a series of recurrent broad jets observed in AR 10484 on 21?24 October 2003. In particular, one of them occurred simultaneously with an M2.4 flare on 23 October at 02:41 UT (SOLA2003-10-23). Both events were observed by the ARIES Hα Solar Tower-Telescope, TRACE, SOHO, and RHESSI instruments. The flare was very impulsive and followed by a narrow CME. A local force-free model of AR 10484 is the basis to compute its topology. We find bald patches (BPs) at the flare site. This BP topology is present for at least two days before to events. Large-scale field lines, associated with the BPs, represent open loops. This is confirmed by a global potential free source surface (PFSS) model. Following the brightest leading edge of the Hα and EUV jet emission, we can temporarily associate these emissions with a narrow CME. Results. Considering their characteristics, the observed broad jets appear to be of the blowout class. As the most plausible scenario, we propose that magnetic reconnection could occur at the BP separatrices forced by the destabilization of a continuously reformed flux rope underlying them. The reconnection process could bring the cool flux-rope material into the reconnected open field lines driving the series of recurrent blowout jets and accompanying CMEs. Conclusions. Based on a model of the coronal field, we compute the AR 10484 topology at the location where flaring and blowout jets occurred from 21 to 24 October 2003. This topology can consistently explain the origin of these events. Fil: Chandra, R.. Kumaun University; India 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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Joshi, B.. Udaipur Solar Observatory; India 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: Cremades Fernandez, Maria Hebe. Universidad Tecnologica Nacional; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia 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: Srivastava, A. K.. Indian Institute Of Technology; India Fil: Uddi, W.. Aryabhatta Research Institute of Observational Sciences; India |
description |
Context. A subclass of broad extreme ultraviolet (EUV) and X-ray jets, called blowout jets, have become a topic of research since they could be the link between standard collimated jets and coronal mass ejections (CMEs). Aims. Our aim is to understand the origin of a series of broad jets, some of which are accompanied by flares and associated with narrow and jet-like CMEs. Methods. We analyze observations of a series of recurrent broad jets observed in AR 10484 on 21?24 October 2003. In particular, one of them occurred simultaneously with an M2.4 flare on 23 October at 02:41 UT (SOLA2003-10-23). Both events were observed by the ARIES Hα Solar Tower-Telescope, TRACE, SOHO, and RHESSI instruments. The flare was very impulsive and followed by a narrow CME. A local force-free model of AR 10484 is the basis to compute its topology. We find bald patches (BPs) at the flare site. This BP topology is present for at least two days before to events. Large-scale field lines, associated with the BPs, represent open loops. This is confirmed by a global potential free source surface (PFSS) model. Following the brightest leading edge of the Hα and EUV jet emission, we can temporarily associate these emissions with a narrow CME. Results. Considering their characteristics, the observed broad jets appear to be of the blowout class. As the most plausible scenario, we propose that magnetic reconnection could occur at the BP separatrices forced by the destabilization of a continuously reformed flux rope underlying them. The reconnection process could bring the cool flux-rope material into the reconnected open field lines driving the series of recurrent blowout jets and accompanying CMEs. Conclusions. Based on a model of the coronal field, we compute the AR 10484 topology at the location where flaring and blowout jets occurred from 21 to 24 October 2003. This topology can consistently explain the origin of these events. |
publishDate |
2017 |
dc.date.none.fl_str_mv |
2017-01 |
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/11336/21704 Chandra, R.; Mandrini, Cristina Hemilse; Schmieder, B.; Joshi, B.; Cristiani, Germán Diego; et al.; Blowouts jets and impulsive eruptive flares in a bald-patch topology; EDP Sciences; Astronomy and Astrophysics; 598; A41; 1-2017; 1-15 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/21704 |
identifier_str_mv |
Chandra, R.; Mandrini, Cristina Hemilse; Schmieder, B.; Joshi, B.; Cristiani, Germán Diego; et al.; Blowouts jets and impulsive eruptive flares in a bald-patch topology; EDP Sciences; Astronomy and Astrophysics; 598; A41; 1-2017; 1-15 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2017/02/aa28984-16/aa28984-16.html info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628984 |
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 |
dc.publisher.none.fl_str_mv |
EDP Sciences |
publisher.none.fl_str_mv |
EDP Sciences |
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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1844614505456205824 |
score |
13.070432 |