A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis
Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapola...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Gary, G. Allen [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| 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), 3 vom: 07. Aug., Seite 847-865 |
|---|---|
| Übergeordnetes Werk: |
volume:289 ; year:2013 ; number:3 ; day:07 ; month:08 ; pages:847-865 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11207-013-0359-8 |
|---|
| Katalog-ID: |
OLC2033615332 |
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| 520 | |a Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. | ||
| 650 | 4 | |a Magnetic fields, models | |
| 650 | 4 | |a Magnetic fields, corona | |
| 650 | 4 | |a Active regions, magnetic fields | |
| 650 | 4 | |a Chromosphere, models | |
| 650 | 4 | |a Instrumentation and data management | |
| 700 | 1 | |a Hu, Qiang |4 aut | |
| 700 | 1 | |a Lee, Jong Kwan |4 aut | |
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10.1007/s11207-013-0359-8 doi (DE-627)OLC2033615332 (DE-He213)s11207-013-0359-8-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Gary, G. Allen verfasserin aut A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. Magnetic fields, models Magnetic fields, corona Active regions, magnetic fields Chromosphere, models Instrumentation and data management Hu, Qiang aut Lee, Jong Kwan aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 3 vom: 07. Aug., Seite 847-865 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:3 day:07 month:08 pages:847-865 https://doi.org/10.1007/s11207-013-0359-8 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 3 07 08 847-865 |
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10.1007/s11207-013-0359-8 doi (DE-627)OLC2033615332 (DE-He213)s11207-013-0359-8-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Gary, G. Allen verfasserin aut A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. Magnetic fields, models Magnetic fields, corona Active regions, magnetic fields Chromosphere, models Instrumentation and data management Hu, Qiang aut Lee, Jong Kwan aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 3 vom: 07. Aug., Seite 847-865 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:3 day:07 month:08 pages:847-865 https://doi.org/10.1007/s11207-013-0359-8 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 3 07 08 847-865 |
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10.1007/s11207-013-0359-8 doi (DE-627)OLC2033615332 (DE-He213)s11207-013-0359-8-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Gary, G. Allen verfasserin aut A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. Magnetic fields, models Magnetic fields, corona Active regions, magnetic fields Chromosphere, models Instrumentation and data management Hu, Qiang aut Lee, Jong Kwan aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 3 vom: 07. Aug., Seite 847-865 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:3 day:07 month:08 pages:847-865 https://doi.org/10.1007/s11207-013-0359-8 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 3 07 08 847-865 |
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10.1007/s11207-013-0359-8 doi (DE-627)OLC2033615332 (DE-He213)s11207-013-0359-8-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Gary, G. Allen verfasserin aut A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. Magnetic fields, models Magnetic fields, corona Active regions, magnetic fields Chromosphere, models Instrumentation and data management Hu, Qiang aut Lee, Jong Kwan aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 3 vom: 07. Aug., Seite 847-865 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:3 day:07 month:08 pages:847-865 https://doi.org/10.1007/s11207-013-0359-8 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 3 07 08 847-865 |
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10.1007/s11207-013-0359-8 doi (DE-627)OLC2033615332 (DE-He213)s11207-013-0359-8-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Gary, G. Allen verfasserin aut A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis 2013 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2013 Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. Magnetic fields, models Magnetic fields, corona Active regions, magnetic fields Chromosphere, models Instrumentation and data management Hu, Qiang aut Lee, Jong Kwan aut Enthalten in Solar physics Springer Netherlands, 1967 289(2013), 3 vom: 07. Aug., Seite 847-865 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:289 year:2013 number:3 day:07 month:08 pages:847-865 https://doi.org/10.1007/s11207-013-0359-8 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 3 07 08 847-865 |
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A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis |
| abstract |
Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. © Springer Science+Business Media Dordrecht 2013 |
| abstractGer |
Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. © Springer Science+Business Media Dordrecht 2013 |
| abstract_unstemmed |
Abstract A rapid and flexible manual method is described that maps individual coronal loops of a 2D EUV image as Bézier curves using only four points per loop. Using the coronal loops as surrogates of magnetic-field lines, the mapping results restrict the magnetic-field models derived from extrapolations of magnetograms to those admissible and inadmissible via a fitness parameter. We outline explicitly how the coronal loops can be employed in constraining competing magnetic-field models by transforming 2D coronal-loop images into 3D field lines. The magnetic-field extrapolations must satisfy not only the lower boundary conditions of the vector field (the vector magnetogram) but also must have a set of field lines that satisfies the mapped coronal loops in the volume, analogous to an upper boundary condition. This method uses the minimization of the misalignment angles between the magnetic-field model and the best set of 3D field lines that match a set of closed coronal loops. The presented method is an important tool in determining the fitness of magnetic-field models for the solar atmosphere. The magnetic-field structure is crucial in determining the overall dynamics of the solar atmosphere. © Springer Science+Business Media Dordrecht 2013 |
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3 |
| title_short |
A Rapid, Manual Method to Map Coronal-Loop Structures of an Active Region Using Cubic Bézier Curves and Its Applications to Misalignment Angle Analysis |
| url |
https://doi.org/10.1007/s11207-013-0359-8 |
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| author2 |
Hu, Qiang Lee, Jong Kwan |
| author2Str |
Hu, Qiang Lee, Jong Kwan |
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| doi_str |
10.1007/s11207-013-0359-8 |
| up_date |
2024-07-03T17:42:58.687Z |
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