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Solar prominences

Published online by Cambridge University Press:  01 September 2008

Brigitte Schmieder ,
Guillaume Aulanier  and
Tibor Török
Brigitte Schmieder
Affiliation:
LESIA, Observatoire de Paris, 5 Place Janssen, Meudon, 92195, France email: [email protected]
Guillaume Aulanier
Affiliation:
LESIA, Observatoire de Paris, 5 Place Janssen, Meudon, 92195, France email: [email protected]
Tibor Török
Affiliation:
LESIA, Observatoire de Paris, 5 Place Janssen, Meudon, 92195, France email: [email protected]
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Abstract

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Solar filaments (or prominences) are magnetic structures in the corona. They can be represented by twisted flux ropes in a bipolar magnetic environment. In such models, the dipped field lines of the flux rope carry the filament material and parasitic polarities in the filament channel are responsible for the existence of the lateral feet of prominences.

Very simple laws do exist for the chirality of filaments, the so-called “filament chirality rules”: commonly dextral/sinistral filaments corresponding to left- (resp. right) hand magnetic twists are in the North/South hemisphere. Combining these rules with 3D weakly twisted flux tube models, the sign of the magnetic helicity in several filaments were identified. These rules were also applied to the 180° disambiguation of the direction of the photospheric transverse magnetic field around filaments using THEMIS vector magnetograph data (López Ariste et al. 2006). Consequently, an unprecedented evidence of horizontal magnetic support in filament feet has been observed, as predicted by former magnetostatic and recent MHD models.

The second part of this review concerns the role of emerging flux in the vicinity of filament channels. It has been suggested that magnetic reconnection between the emerging flux and the pre-existing coronal field can trigger filament eruptions and CMEs. For a particular event, observed with Hinode/XRT, we observe signatures of such a reconnection, but no eruption of the filament. We present a 3D numerical simulation of emerging flux in the vicinity of a flux rope which was performed to reproduce this event and we briefly discuss, based on the simulation results, why the filament did not erupt.

Keywords

Solar prominencemagnetic emerging fluxeruption3D MHD model
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 223 - 232
Copyright
Copyright © International Astronomical Union 2009

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