Multi-scale reconnections in a complex CME

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A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, a...

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Autores principales: van Driel-Gesztelyi, L., Goff, C.P., Démoulin, P., Culhane, J.L., Matthews, S.A., Harra, L.K., Mandrini, C.H., Klein, K.-L., Kurokawa, H.
Formato: JOUR
Materias:
Magnetic reconnection
Radio burst
Sun: coronal mass ejection
Sun: EUV
Sun: flares
Sun: magnetic fields
Sun: radio
Astrophysics
Crystallography
Magnetic fields
Magnetic materials
Magnetic structure
Field lines
Flux ropes
Magnetic (CE)
Magnetic loops
Magnetic reconnection (MR)
Magnetic-field lines
MDI magnetograms
Multi scaling
Open field lines
radio bursts
radio observations
Radio wavelengths
Solar radius
Magnetism
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_02731177_v42_n5_p858_vanDrielGesztelyi
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_02731177_v42_n5_p858_vanDrielGesztelyi
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spelling todo:paper_02731177_v42_n5_p858_vanDrielGesztelyi2023-10-03T15:15:38Z Multi-scale reconnections in a complex CME van Driel-Gesztelyi, L. Goff, C.P. Démoulin, P. Culhane, J.L. Matthews, S.A. Harra, L.K. Mandrini, C.H. Klein, K.-L. Kurokawa, H. Magnetic reconnection Radio burst Sun: coronal mass ejection Sun: EUV Sun: flares Sun: magnetic fields Sun: radio Astrophysics Crystallography Magnetic fields Magnetic materials Magnetic structure Field lines Flux ropes Magnetic (CE) Magnetic loops Magnetic reconnection (MR) Magnetic-field lines MDI magnetograms Multi scaling Open field lines radio bursts radio observations Radio wavelengths Solar radius Magnetism A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, and radio observations from Culgoora and Wind/ WAVES to understand the complex development of this event. We reach three main conclusions. First, we link the first two impulsive flares to tether-cutting reconnections and the launch of the CME. This complex observation shows that impulsive quadrupolar flares can be eruptive. Second, we relate the last of the flares, an LDE, to the relaxation phase following forced reconnections between the erupting flux rope and neighbouring magnetic field lines, when reconnection reverses and restores some of the pre-eruption magnetic connectivities. Finally, we show that reconnection with the magnetic structure of a previous CME launched about 8 h earlier injects electrons into open field lines having a local dip and apex (located at about six solar radii height). This is observed as an N-burst at decametre radio wavelengths. The dipped shape of these field lines is due to large-scale magnetic reconnection between expanding magnetic loops and open field lines of a neighbouring streamer. This particular situation explains why this is the first N-burst ever observed at long radio wavelengths. © 2007 COSPAR. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_02731177_v42_n5_p858_vanDrielGesztelyi
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Magnetic reconnection
Radio burst
Sun: coronal mass ejection
Sun: EUV
Sun: flares
Sun: magnetic fields
Sun: radio
Astrophysics
Crystallography
Magnetic fields
Magnetic materials
Magnetic structure
Field lines
Flux ropes
Magnetic (CE)
Magnetic loops
Magnetic reconnection (MR)
Magnetic-field lines
MDI magnetograms
Multi scaling
Open field lines
radio bursts
radio observations
Radio wavelengths
Solar radius
Magnetism
spellingShingle Magnetic reconnection
Radio burst
Sun: coronal mass ejection
Sun: EUV
Sun: flares
Sun: magnetic fields
Sun: radio
Astrophysics
Crystallography
Magnetic fields
Magnetic materials
Magnetic structure
Field lines
Flux ropes
Magnetic (CE)
Magnetic loops
Magnetic reconnection (MR)
Magnetic-field lines
MDI magnetograms
Multi scaling
Open field lines
radio bursts
radio observations
Radio wavelengths
Solar radius
Magnetism
van Driel-Gesztelyi, L.
Goff, C.P.
Démoulin, P.
Culhane, J.L.
Matthews, S.A.
Harra, L.K.
Mandrini, C.H.
Klein, K.-L.
Kurokawa, H.
Multi-scale reconnections in a complex CME
topic_facet Magnetic reconnection
Radio burst
Sun: coronal mass ejection
Sun: EUV
Sun: flares
Sun: magnetic fields
Sun: radio
Astrophysics
Crystallography
Magnetic fields
Magnetic materials
Magnetic structure
Field lines
Flux ropes
Magnetic (CE)
Magnetic loops
Magnetic reconnection (MR)
Magnetic-field lines
MDI magnetograms
Multi scaling
Open field lines
radio bursts
radio observations
Radio wavelengths
Solar radius
Magnetism
description A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, and radio observations from Culgoora and Wind/ WAVES to understand the complex development of this event. We reach three main conclusions. First, we link the first two impulsive flares to tether-cutting reconnections and the launch of the CME. This complex observation shows that impulsive quadrupolar flares can be eruptive. Second, we relate the last of the flares, an LDE, to the relaxation phase following forced reconnections between the erupting flux rope and neighbouring magnetic field lines, when reconnection reverses and restores some of the pre-eruption magnetic connectivities. Finally, we show that reconnection with the magnetic structure of a previous CME launched about 8 h earlier injects electrons into open field lines having a local dip and apex (located at about six solar radii height). This is observed as an N-burst at decametre radio wavelengths. The dipped shape of these field lines is due to large-scale magnetic reconnection between expanding magnetic loops and open field lines of a neighbouring streamer. This particular situation explains why this is the first N-burst ever observed at long radio wavelengths. © 2007 COSPAR.
format JOUR
author van Driel-Gesztelyi, L.
Goff, C.P.
Démoulin, P.
Culhane, J.L.
Matthews, S.A.
Harra, L.K.
Mandrini, C.H.
Klein, K.-L.
Kurokawa, H.
author_facet van Driel-Gesztelyi, L.
Goff, C.P.
Démoulin, P.
Culhane, J.L.
Matthews, S.A.
Harra, L.K.
Mandrini, C.H.
Klein, K.-L.
Kurokawa, H.
author_sort van Driel-Gesztelyi, L.
title Multi-scale reconnections in a complex CME
title_short Multi-scale reconnections in a complex CME
title_full Multi-scale reconnections in a complex CME
title_fullStr Multi-scale reconnections in a complex CME
title_full_unstemmed Multi-scale reconnections in a complex CME
title_sort multi-scale reconnections in a complex cme
url http://hdl.handle.net/20.500.12110/paper_02731177_v42_n5_p858_vanDrielGesztelyi
work_keys_str_mv AT vandrielgesztelyil multiscalereconnectionsinacomplexcme
AT goffcp multiscalereconnectionsinacomplexcme
AT demoulinp multiscalereconnectionsinacomplexcme
AT culhanejl multiscalereconnectionsinacomplexcme
AT matthewssa multiscalereconnectionsinacomplexcme
AT harralk multiscalereconnectionsinacomplexcme
AT mandrinich multiscalereconnectionsinacomplexcme
AT kleinkl multiscalereconnectionsinacomplexcme
AT kurokawah multiscalereconnectionsinacomplexcme
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