Abstract
We suggest the following heuristic model for the evolution of a quiescent filament. The middle part of the filament rises due to heating, while its ends remain anchored in the chromosphere; and a kink appears in the Hα filament due to projection and line-of-sight effects. Further, the top segment of the filament rises rapidly above the solar surface 1–2 days before the disappearance of a filament or eruption of a prominence. The top of the filament attains a high temperature due to further heating, thereby becoming invisible in Hα, giving the impression that the filament has split into two parts. It is expected that this gap between the Hα filament can be seen in the observations in high-temperature lines and soft X-rays.
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