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Abstract
Aims. We investigate the formation of flux ropes in a flux emergence region and their rise into the outer atmosphere of the Sun.
Methods. We perform 3D numerical experiments by solving the time-dependent and resistive MHD equations.
Results. A sub-photospheric twisted flux tube rises from the solar interior and expands into the corona. A flux rope is formed within the expanding field, due to shearing and reconnection of field lines at low atmospheric heights. If the tube emerges into a non-magnetized atmosphere, the flux rope rises, but remains confined inside the expanding magnetized volume. In contrast, if the expanding tube is allowed to reconnect with a pre-existing coronal field, the flux rope experiences a full eruption with a rise profile that is in qualitative agreement with erupting filaments and Coronal Mass Ejections.
Original language | English |
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Number of pages | 4 |
Journal | Experimental Astronomy |
Volume | 492 |
DOIs | |
Publication status | Published - Dec 2008 |
Keywords
- magnetohydrodynamics (MHD)
- methods: numerical
- Sun: activity
- Sun: corona
- Sun: magnetic fields
- CORONAL MASS EJECTIONS
- HELICITY BUDGET
- EMERGING FLUX
- FIELD
- KINK
- ACCELERATION
- FILAMENT
- REGIONS
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Dive into the research topics of 'Eruption of magnetic flux ropes during flux emergence'. Together they form a unique fingerprint.Projects
- 1 Finished
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Solar&Magnetospheric Plasma Theory PP/E1: Solar and Magnetospheric Plasma Theory
Neukirch, T. (PI), Hood, A. W. (CoI), Parnell, C. E. (CoI), Priest, E. (CoI), Roberts, B. (CoI) & Wright, A. N. (CoI)
1/04/07 → 31/03/12
Project: Standard