An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event
Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations...
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| Autor*in: |
Prise, A. J. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2013 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science+Business Media Dordrecht 2013 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Springer Netherlands, 1967, 289(2013), 5 vom: 16. Nov., Seite 1731-1744 |
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| Übergeordnetes Werk: |
volume:289 ; year:2013 ; number:5 ; day:16 ; month:11 ; pages:1731-1744 |
| Links: |
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| DOI / URN: |
10.1007/s11207-013-0435-0 |
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OLC2033615847 |
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| 520 | |a Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. | ||
| 650 | 4 | |a Coronal Mass Ejection | |
| 650 | 4 | |a Radio Burst | |
| 650 | 4 | |a Solar Energetic Particle | |
| 650 | 4 | |a Solar Energetic Particle Event | |
| 650 | 4 | |a Stereo Spacecraft | |
| 700 | 1 | |a Harra, L. K. |4 aut | |
| 700 | 1 | |a Matthews, S. A. |4 aut | |
| 700 | 1 | |a Long, D. M. |4 aut | |
| 700 | 1 | |a Aylward, A. D. |4 aut | |
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10.1007/s11207-013-0435-0 doi (DE-627)OLC2033615847 (DE-He213)s11207-013-0435-0-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Prise, A. J. verfasserin aut An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. Coronal Mass Ejection Radio Burst Solar Energetic Particle Solar Energetic Particle Event Stereo Spacecraft Harra, L. K. aut Matthews, S. A. aut Long, D. M. aut Aylward, A. D. aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 5 vom: 16. Nov., Seite 1731-1744 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:5 day:16 month:11 pages:1731-1744 https://doi.org/10.1007/s11207-013-0435-0 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 289 2013 5 16 11 1731-1744 |
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10.1007/s11207-013-0435-0 doi (DE-627)OLC2033615847 (DE-He213)s11207-013-0435-0-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Prise, A. J. verfasserin aut An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. Coronal Mass Ejection Radio Burst Solar Energetic Particle Solar Energetic Particle Event Stereo Spacecraft Harra, L. K. aut Matthews, S. A. aut Long, D. M. aut Aylward, A. D. aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 5 vom: 16. Nov., Seite 1731-1744 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:5 day:16 month:11 pages:1731-1744 https://doi.org/10.1007/s11207-013-0435-0 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 289 2013 5 16 11 1731-1744 |
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10.1007/s11207-013-0435-0 doi (DE-627)OLC2033615847 (DE-He213)s11207-013-0435-0-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Prise, A. J. verfasserin aut An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. Coronal Mass Ejection Radio Burst Solar Energetic Particle Solar Energetic Particle Event Stereo Spacecraft Harra, L. K. aut Matthews, S. A. aut Long, D. M. aut Aylward, A. D. aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 5 vom: 16. Nov., Seite 1731-1744 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:5 day:16 month:11 pages:1731-1744 https://doi.org/10.1007/s11207-013-0435-0 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 289 2013 5 16 11 1731-1744 |
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10.1007/s11207-013-0435-0 doi (DE-627)OLC2033615847 (DE-He213)s11207-013-0435-0-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Prise, A. J. verfasserin aut An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. Coronal Mass Ejection Radio Burst Solar Energetic Particle Solar Energetic Particle Event Stereo Spacecraft Harra, L. K. aut Matthews, S. A. aut Long, D. M. aut Aylward, A. D. aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 5 vom: 16. Nov., Seite 1731-1744 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:5 day:16 month:11 pages:1731-1744 https://doi.org/10.1007/s11207-013-0435-0 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 289 2013 5 16 11 1731-1744 |
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10.1007/s11207-013-0435-0 doi (DE-627)OLC2033615847 (DE-He213)s11207-013-0435-0-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Prise, A. J. verfasserin aut An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. Coronal Mass Ejection Radio Burst Solar Energetic Particle Solar Energetic Particle Event Stereo Spacecraft Harra, L. K. aut Matthews, S. A. aut Long, D. M. aut Aylward, A. D. aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 5 vom: 16. Nov., Seite 1731-1744 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:5 day:16 month:11 pages:1731-1744 https://doi.org/10.1007/s11207-013-0435-0 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 289 2013 5 16 11 1731-1744 |
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An Investigation of the CME of 3 November 2011 and Its Associated Widespread Solar Energetic Particle Event |
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Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. © Springer Science+Business Media Dordrecht 2013 |
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Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. © Springer Science+Business Media Dordrecht 2013 |
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Abstract Multi-spacecraft observations are used to study the in-situ effects of a large coronal mass ejection (CME) erupting from the farside of the Sun on 3 November 2011, with particular emphasis on the associated solar energetic particle (SEP) event. At that time both Solar Terrestrial Relations Observatory (STEREO) spacecraft were located more than 90 degrees from Earth and could observe the CME eruption directly, with the CME visible on-disk from STEREO-B and off the limb from STEREO-A. Signatures of pressure variations in the corona such as deflected streamers were seen, indicating the presence of a coronal shock associated with this CME eruption. The evolution of the CME and an associated extreme-ultraviolet (EUV) wave were studied using EUV and coronagraph images. It was found that the lateral expansion of the CME low in the corona closely tracked the propagation of the EUV wave, with measured velocities of 240±19 km $ s^{−1} $ and 221±15 km $ s^{−1} $ for the CME and wave, respectively. Solar energetic particles were observed to arrive first at STEREO-A, followed by electrons at the Wind spacecraft at $ L_{1} $, then STEREO-B, and finally protons arrived simultaneously at Wind and STEREO-B. By carrying out a velocity-dispersion analysis on the particles arriving at each location, it was found that energetic particles arriving at STEREO-A were released first and that the release of particles arriving at STEREO-B was delayed by about 50 minutes. Analysis of the expansion of the CME to a wider longitude range indicates that this delay is a result of the time taken for the CME edge to reach the footpoints of the magnetic-field lines connected to STEREO-B. The CME expansion is not seen to reach the magnetic footpoint of Wind at the time of solar-particle release for the particles detected here, suggesting that these particles may not be associated with this CME. © Springer Science+Business Media Dordrecht 2013 |
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