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Observations of the early rise and propagation phases of solar eruptiveprominences can provide clues about the forces acting on them through thebehavior of their acceleration with height. We have analyzed such an event,observed on 13 April 2010 by SWAP on PROBA2 and EUVI on STEREO. A feature atthe top of the erupting prominence was identified and tracked in images fromthe three spacecraft. The triangulation technique was used to derive the truedirection of propagation of this feature. The reconstructed points were fittedwith two mathematical models: i) a power-law polynomial function and ii) acubic smoothing spline, in order to derive the accelerations. The first modelis characterized by five degrees of freedom while the second one ischaracterized by ten degrees of freedom. The results show that the accelerationincreases smoothly and it is continuously increasing with height. We concludethat the prominence is not accelerated immediately by local reconnection butrather is swept away as part of a large-scale relaxation of the coronalmagnetic field.

Study of a Prominence Eruption using PROBA2/SWAP and STEREO/EUVI Data