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

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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 t...

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Autores principales: Mandrini, C.H., Pohjolainen, S., Dasso, S., Green, L.M., Démoulin, P., Van Driel-Gesztelyi, L., Copperwheat, C., Foley, C.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2005
Materias:
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)
Wind spacecrafts
Astrophysics
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v434_n2_p725_Mandrini
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paperaa:paper_00046361_v434_n2_p725_Mandrini
record_format dspace
spelling paperaa:paper_00046361_v434_n2_p725_Mandrini2023-06-12T16:40:46Z Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed Astron. Astrophys. 2005;434(2):725-740 Mandrini, C.H. Pohjolainen, S. Dasso, S. Green, L.M. Démoulin, P. Van Driel-Gesztelyi, L. Copperwheat, C. Foley, C. 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 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. 2005 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v434_n2_p725_Mandrini
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language Inglés
orig_language_str_mv eng
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
spellingShingle 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
Mandrini, C.H.
Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
topic_facet 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
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.
format Artículo
Artículo
publishedVersion
author Mandrini, C.H.
Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
author_facet Mandrini, C.H.
Pohjolainen, S.
Dasso, S.
Green, L.M.
Démoulin, P.
Van Driel-Gesztelyi, L.
Copperwheat, C.
Foley, C.
author_sort Mandrini, C.H.
title Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed
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
publishDate 2005
url http://hdl.handle.net/20.500.12110/paper_00046361_v434_n2_p725_Mandrini
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