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Abstract
Coronal flux ropes are highly sheared or twisted magnetic fields overlying polarity inversion lines on the solar photosphere. The formation of such flux ropes is briefly discussed. A coronal flux rope can be stable for many days and then suddenly lose equilibrium and erupt, producing a coronal mass ejection (CME). To understand what causes such eruptions, we need to determine the 3D magnetic structure of observed active regions prior to CMEs. This requires constructing nonlinear force free field models of active regions based on observed photospheric vector fields, H alpha filaments, or coronal loop structures. We describe a new method for constructing models containing flux ropes. (c) 2006 Elsevier Ltd. All rights reserved.
Original language | English |
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Pages (from-to) | 24-31 |
Number of pages | 8 |
Journal | Journal of Atmospheric and Solar-Terrestrial Physics |
Volume | 69 |
DOIs | |
Publication status | Published - Feb 2007 |
Keywords
- solar corona
- solar magnetic fields
- coronal mass ejections
- solar prominences
- CONFIGURATIONS SUPPORTING PROMINENCES
- FORCE-FREE
- ACTIVE-REGION
- QUIESCENT PROMINENCES
- HEMISPHERIC PATTERN
- FILAMENT CHANNEL
- LATERAL FEET
- FIELDS
- EVOLUTION
- HELICITY
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Dive into the research topics of 'Modeling magnetic flux ropes in the solar atmosphere'. Together they form a unique fingerprint.Projects
- 1 Finished
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PPARC FELOWSHIP-D MACKAY: Dynamic Solar Magnitude Fields
Mackay, D. H. (PI)
1/10/04 → 30/09/09
Project: Standard