On the eruption of prominences and disappearance of quiescent filaments

Details On the eruption of prominences and disappearance of quiescent filaments On the eruption of prominences and disappearance of quiescent filaments

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..158..259s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 158, no. 2, p. 259-268

Physics

10

Dynamic Stability, Solar Physics, Solar Prominences, Sun, Thermal Stability, Chromosphere, H Alpha Line, Heating, Solar X-Rays

Scientific paper

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 H alpha 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 H alpha, giving the impression that the filament has slit into two parts. It is expected that this gap between the H alpha filament can be seen in the observations in high-temperature lines and soft X-rays.

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