Abstract
Many active and short-lived dynamic structures in the solar atmosphere (such as sprays, surges and active prominences) are responsible for transportation of mass and energy into the solar corona, although the contribution of each event is not the same. At the same time, this kind of plasma ejections owe their existence to local magnetic fields. One of the above mentioned phenomena is eruptive prominence. According to Schmieder (1988), common characteristics of eruptive prominences are helical structures, the rotational motions and ‘twisting’ or ‘detwisting’ of the fine structural threads.In this paper, our aim is to show the evolution of a detwisting prominence event and to present to the readers a new data treatment method which can be used to study this kind of event more precisely and rapidly.
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