Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed

Autores
Mandrini, C.H.; Pohjolainen, S.; Dasso, S.; Green, L.M.; Démoulin, P.; Van Driel-Gesztelyi, L.; Copperwheat, C.; Foley, C.
Año de publicación
2005
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Using multi-instrument and multi-wavelength observations (SOHO/MDI and BIT, TRACE and Yohkoh/SXT), as well as computing the coronal magnetic field of a tiny bipole combined with modelling of Wind in situ data, we provide evidences for the smallest event ever observed which links a sigmoid eruption to an interplanetary magnetic cloud (MC). The tiny bipole, which was observed very close to the solar disc centre, had a factor one hundred less flux than a classical active region (AR). In the corona it had a sigmoidal structure, observed mainly in EUV, and we found a very high level of non-potentiality in the modelled magnetic field, 10 times higher than we have ever found in any AR. From May 11, 1998, and until its disappearance, the sigmoid underwent three intense impulsive events. The largest of these events had extended EUV dimmings and a cusp. The Wind spacecraft detected 4.5 days later one of the smallest MC ever identified (about a factor one hundred times less magnetic flux in the axial component than that of an average MC). The link between this last eruption and the interplanetary magnetic cloud is supported by several pieces of evidence: good timing, same coronal loop and MC orientation, same magnetic field direction and magnetic helicity sign in the coronal loops and in the MC. We further quantify this link by estimating the magnetic flux (measured in the dimming regions and in the MC) and the magnetic helicity (pre- to post-event change in the solar corona and helicity content of the MC). Within the uncertainties, both magnetic fluxes and helicities are in reasonable agreement, which brings further evidences of their link. These observations show that the ejections of tiny magnetic flux ropes are indeed possible and put new constraints on CME models. © ESO 2005.
Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astron. Astrophys. 2005;434(2):725-740
Materia
Sun: corona
Sun: magnetic fields
Interplanetary spacecraft
Magnetic field effects
Magnetic flux
Magnetic moments
Planets
Statistical methods
Wind effects
X rays
Coronal mass ejections (CME)
Sun: corona
Sun: magnetic fields
Wind spacecrafts
Astrophysics
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_00046361_v434_n2_p725_Mandrini

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oai_identifier_str paperaa:paper_00046361_v434_n2_p725_Mandrini
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observedMandrini, C.H.Pohjolainen, S.Dasso, S.Green, L.M.Démoulin, P.Van Driel-Gesztelyi, L.Copperwheat, C.Foley, C.Sun: coronaSun: magnetic fieldsInterplanetary spacecraftMagnetic field effectsMagnetic fluxMagnetic momentsPlanetsStatistical methodsWind effectsX raysCoronal mass ejections (CME)Sun: coronaSun: magnetic fieldsWind spacecraftsAstrophysicsUsing multi-instrument and multi-wavelength observations (SOHO/MDI and BIT, TRACE and Yohkoh/SXT), as well as computing the coronal magnetic field of a tiny bipole combined with modelling of Wind in situ data, we provide evidences for the smallest event ever observed which links a sigmoid eruption to an interplanetary magnetic cloud (MC). The tiny bipole, which was observed very close to the solar disc centre, had a factor one hundred less flux than a classical active region (AR). In the corona it had a sigmoidal structure, observed mainly in EUV, and we found a very high level of non-potentiality in the modelled magnetic field, 10 times higher than we have ever found in any AR. From May 11, 1998, and until its disappearance, the sigmoid underwent three intense impulsive events. The largest of these events had extended EUV dimmings and a cusp. The Wind spacecraft detected 4.5 days later one of the smallest MC ever identified (about a factor one hundred times less magnetic flux in the axial component than that of an average MC). The link between this last eruption and the interplanetary magnetic cloud is supported by several pieces of evidence: good timing, same coronal loop and MC orientation, same magnetic field direction and magnetic helicity sign in the coronal loops and in the MC. We further quantify this link by estimating the magnetic flux (measured in the dimming regions and in the MC) and the magnetic helicity (pre- to post-event change in the solar corona and helicity content of the MC). Within the uncertainties, both magnetic fluxes and helicities are in reasonable agreement, which brings further evidences of their link. These observations show that the ejections of tiny magnetic flux ropes are indeed possible and put new constraints on CME models. © ESO 2005.Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.2005info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://hdl.handle.net/20.500.12110/paper_00046361_v434_n2_p725_MandriniAstron. Astrophys. 2005;434(2):725-740reponame:Biblioteca Digital (UBA-FCEN)instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesinstacron:UBA-FCENenginfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/2.5/ar2025-09-29T13:42:55Zpaperaa:paper_00046361_v434_n2_p725_MandriniInstitucionalhttps://digital.bl.fcen.uba.ar/Universidad públicaNo correspondehttps://digital.bl.fcen.uba.ar/cgi-bin/oaiserver.cgiana@bl.fcen.uba.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:18962025-09-29 13:42:56.458Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
title Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
spellingShingle Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
Mandrini, C.H.
Sun: corona
Sun: magnetic fields
Interplanetary spacecraft
Magnetic field effects
Magnetic flux
Magnetic moments
Planets
Statistical methods
Wind effects
X rays
Coronal mass ejections (CME)
Sun: corona
Sun: magnetic fields
Wind spacecrafts
Astrophysics
title_short Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
title_full Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
title_fullStr Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
title_full_unstemmed Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
title_sort Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
dc.creator.none.fl_str_mv Mandrini, C.H.
Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
author Mandrini, C.H.
author_facet Mandrini, C.H.
Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
author_role author
author2 Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Sun: corona
Sun: magnetic fields
Interplanetary spacecraft
Magnetic field effects
Magnetic flux
Magnetic moments
Planets
Statistical methods
Wind effects
X rays
Coronal mass ejections (CME)
Sun: corona
Sun: magnetic fields
Wind spacecrafts
Astrophysics
topic Sun: corona
Sun: magnetic fields
Interplanetary spacecraft
Magnetic field effects
Magnetic flux
Magnetic moments
Planets
Statistical methods
Wind effects
X rays
Coronal mass ejections (CME)
Sun: corona
Sun: magnetic fields
Wind spacecrafts
Astrophysics
dc.description.none.fl_txt_mv Using multi-instrument and multi-wavelength observations (SOHO/MDI and BIT, TRACE and Yohkoh/SXT), as well as computing the coronal magnetic field of a tiny bipole combined with modelling of Wind in situ data, we provide evidences for the smallest event ever observed which links a sigmoid eruption to an interplanetary magnetic cloud (MC). The tiny bipole, which was observed very close to the solar disc centre, had a factor one hundred less flux than a classical active region (AR). In the corona it had a sigmoidal structure, observed mainly in EUV, and we found a very high level of non-potentiality in the modelled magnetic field, 10 times higher than we have ever found in any AR. From May 11, 1998, and until its disappearance, the sigmoid underwent three intense impulsive events. The largest of these events had extended EUV dimmings and a cusp. The Wind spacecraft detected 4.5 days later one of the smallest MC ever identified (about a factor one hundred times less magnetic flux in the axial component than that of an average MC). The link between this last eruption and the interplanetary magnetic cloud is supported by several pieces of evidence: good timing, same coronal loop and MC orientation, same magnetic field direction and magnetic helicity sign in the coronal loops and in the MC. We further quantify this link by estimating the magnetic flux (measured in the dimming regions and in the MC) and the magnetic helicity (pre- to post-event change in the solar corona and helicity content of the MC). Within the uncertainties, both magnetic fluxes and helicities are in reasonable agreement, which brings further evidences of their link. These observations show that the ejections of tiny magnetic flux ropes are indeed possible and put new constraints on CME models. © ESO 2005.
Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
description Using multi-instrument and multi-wavelength observations (SOHO/MDI and BIT, TRACE and Yohkoh/SXT), as well as computing the coronal magnetic field of a tiny bipole combined with modelling of Wind in situ data, we provide evidences for the smallest event ever observed which links a sigmoid eruption to an interplanetary magnetic cloud (MC). The tiny bipole, which was observed very close to the solar disc centre, had a factor one hundred less flux than a classical active region (AR). In the corona it had a sigmoidal structure, observed mainly in EUV, and we found a very high level of non-potentiality in the modelled magnetic field, 10 times higher than we have ever found in any AR. From May 11, 1998, and until its disappearance, the sigmoid underwent three intense impulsive events. The largest of these events had extended EUV dimmings and a cusp. The Wind spacecraft detected 4.5 days later one of the smallest MC ever identified (about a factor one hundred times less magnetic flux in the axial component than that of an average MC). The link between this last eruption and the interplanetary magnetic cloud is supported by several pieces of evidence: good timing, same coronal loop and MC orientation, same magnetic field direction and magnetic helicity sign in the coronal loops and in the MC. We further quantify this link by estimating the magnetic flux (measured in the dimming regions and in the MC) and the magnetic helicity (pre- to post-event change in the solar corona and helicity content of the MC). Within the uncertainties, both magnetic fluxes and helicities are in reasonable agreement, which brings further evidences of their link. These observations show that the ejections of tiny magnetic flux ropes are indeed possible and put new constraints on CME models. © ESO 2005.
publishDate 2005
dc.date.none.fl_str_mv 2005
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/20.500.12110/paper_00046361_v434_n2_p725_Mandrini
url http://hdl.handle.net/20.500.12110/paper_00046361_v434_n2_p725_Mandrini
dc.language.none.fl_str_mv eng
language eng
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/2.5/ar
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/2.5/ar
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv Astron. Astrophys. 2005;434(2):725-740
reponame:Biblioteca Digital (UBA-FCEN)
instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron:UBA-FCEN
reponame_str Biblioteca Digital (UBA-FCEN)
collection Biblioteca Digital (UBA-FCEN)
instname_str Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron_str UBA-FCEN
institution UBA-FCEN
repository.name.fl_str_mv Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
repository.mail.fl_str_mv ana@bl.fcen.uba.ar
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