Companion Event and Precursor of the X17 Flare on 28 October 2003
Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We f...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Mandrini, C. H. [verfasserIn] |
|---|
| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2006 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science + Business Media, Inc. 2006 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 238(2006), 2 vom: Nov., Seite 293-312 |
|---|---|
| Übergeordnetes Werk: |
volume:238 ; year:2006 ; number:2 ; month:11 ; pages:293-312 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11207-006-0205-3 |
|---|
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OLC2033601021 |
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| 520 | |a Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. | ||
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| 700 | 1 | |a Pariat, E. |4 aut | |
| 700 | 1 | |a Uddin, W. |4 aut | |
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10.1007/s11207-006-0205-3 doi (DE-627)OLC2033601021 (DE-He213)s11207-006-0205-3-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mandrini, C. H. verfasserin aut Companion Event and Precursor of the X17 Flare on 28 October 2003 2006 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science + Business Media, Inc. 2006 Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. Solar Phys Magnetic Reconnection Null Point Reconnection Process Trace Image Demoulin, P. aut Schmieder, B. aut Deluca, E. E. aut Pariat, E. aut Uddin, W. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 238(2006), 2 vom: Nov., Seite 293-312 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:238 year:2006 number:2 month:11 pages:293-312 https://doi.org/10.1007/s11207-006-0205-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 238 2006 2 11 293-312 |
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10.1007/s11207-006-0205-3 doi (DE-627)OLC2033601021 (DE-He213)s11207-006-0205-3-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mandrini, C. H. verfasserin aut Companion Event and Precursor of the X17 Flare on 28 October 2003 2006 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science + Business Media, Inc. 2006 Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. Solar Phys Magnetic Reconnection Null Point Reconnection Process Trace Image Demoulin, P. aut Schmieder, B. aut Deluca, E. E. aut Pariat, E. aut Uddin, W. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 238(2006), 2 vom: Nov., Seite 293-312 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:238 year:2006 number:2 month:11 pages:293-312 https://doi.org/10.1007/s11207-006-0205-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 238 2006 2 11 293-312 |
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10.1007/s11207-006-0205-3 doi (DE-627)OLC2033601021 (DE-He213)s11207-006-0205-3-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mandrini, C. H. verfasserin aut Companion Event and Precursor of the X17 Flare on 28 October 2003 2006 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science + Business Media, Inc. 2006 Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. Solar Phys Magnetic Reconnection Null Point Reconnection Process Trace Image Demoulin, P. aut Schmieder, B. aut Deluca, E. E. aut Pariat, E. aut Uddin, W. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 238(2006), 2 vom: Nov., Seite 293-312 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:238 year:2006 number:2 month:11 pages:293-312 https://doi.org/10.1007/s11207-006-0205-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 238 2006 2 11 293-312 |
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10.1007/s11207-006-0205-3 doi (DE-627)OLC2033601021 (DE-He213)s11207-006-0205-3-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mandrini, C. H. verfasserin aut Companion Event and Precursor of the X17 Flare on 28 October 2003 2006 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science + Business Media, Inc. 2006 Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. Solar Phys Magnetic Reconnection Null Point Reconnection Process Trace Image Demoulin, P. aut Schmieder, B. aut Deluca, E. E. aut Pariat, E. aut Uddin, W. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 238(2006), 2 vom: Nov., Seite 293-312 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:238 year:2006 number:2 month:11 pages:293-312 https://doi.org/10.1007/s11207-006-0205-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 238 2006 2 11 293-312 |
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10.1007/s11207-006-0205-3 doi (DE-627)OLC2033601021 (DE-He213)s11207-006-0205-3-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mandrini, C. H. verfasserin aut Companion Event and Precursor of the X17 Flare on 28 October 2003 2006 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science + Business Media, Inc. 2006 Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. Solar Phys Magnetic Reconnection Null Point Reconnection Process Trace Image Demoulin, P. aut Schmieder, B. aut Deluca, E. E. aut Pariat, E. aut Uddin, W. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 238(2006), 2 vom: Nov., Seite 293-312 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:238 year:2006 number:2 month:11 pages:293-312 https://doi.org/10.1007/s11207-006-0205-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 238 2006 2 11 293-312 |
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Companion Event and Precursor of the X17 Flare on 28 October 2003 |
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Mandrini, C. H. |
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Solar physics |
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Solar physics |
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eng |
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500 - Science |
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2006 |
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293 |
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Mandrini, C. H. Demoulin, P. Schmieder, B. Deluca, E. E. Pariat, E. Uddin, W. |
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238 |
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Mandrini, C. H. |
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10.1007/s11207-006-0205-3 |
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530 |
| title_sort |
companion event and precursor of the x17 flare on 28 october 2003 |
| title_auth |
Companion Event and Precursor of the X17 Flare on 28 October 2003 |
| abstract |
Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. © Springer Science + Business Media, Inc. 2006 |
| abstractGer |
Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. © Springer Science + Business Media, Inc. 2006 |
| abstract_unstemmed |
Abstract A major two-ribbon X17 flare occurred on 28 October 2003, starting at 11:01 UT in active region NOAA 10486. This flare was accompanied by the eruption of a filament and by one of the fastest halo coronal mass ejections registered during the October–November 2003 strong activity period. We focus on the analysis of magnetic field (SOHO/MDI), chromospheric (NainiTal observatory and TRACE), and coronal (TRACE) data obtained before and during the 28 October event. By combining our data analysis with a model of the coronal magnetic field, we concentrate on the study of two events starting before the main flare. One of these events, evident in TRACE images around one hour prior to the main flare, involves a localized magnetic reconnection process associated with the presence of a coronal magnetic null point. This event extends as long as the major flare and we conclude that it is independent from it. A second event, visible in Hα and TRACE images, simultaneous with the previous one, involves a large-scale quadrupolar reconnection process that contributes to decrease the magnetic field tension in the overlaying field configuration; this allows the filament to erupt in a way similar to that proposed by the breakout model, but with magnetic reconnection occurring at Quasi-Separatrix Layers (QSLs) rather than at a magnetic null point. © Springer Science + Business Media, Inc. 2006 |
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Companion Event and Precursor of the X17 Flare on 28 October 2003 |
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Demoulin, P. Schmieder, B. Deluca, E. E. Pariat, E. Uddin, W. |
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