In this thesis I give a brief introduction of the magnetic field configuration of filament (also called prominences) and possible driving mechanisms of filament instability, and then we concentrate on eruption of kinking filament. A kinking filament with their warped axes, generally regarded as the 'fingerprint' of the MHD helical kink instability, are known as a characteristic three-dimension (3D) structure. Therefore, we summary the 3D reconnection technology by using data from the Extreme UltraViolet Image (EUVI) included in SECCHI Aboard twin STEREO spacescrafts and different kinds of 3D filament structures having been reported. A erupting filament, observed by the Extreme Ultraviolet Imager telescope aboard the STEREO spacecraft, exhibited a kinking structure and tilting motion On 5 April 2008. By using three-dimension (3D) reconstruction technology, I obtain the 3D topology for the kinked prominence when its apex arrived at 1.4 radii. By comparing the 3D structure with the magnetic-field configuration computed by using the Potential-Field Source-Surface (PFSS) model, it is suggested that the filament erupted against the rather weaker than stronger overlying magnetic field, which make it appear to tilt toward one side.
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