Solar filaments are long thin threads of relatively dense cool mostly-ionised gas suspended in the million-degree totally-ionised corona. Because filaments are about a hundred times denser than the ambient corona, they should submerge into the chromosphere below, where the density and temperature are similar to their own. Instead, filaments can remain suspended in the corona for a long time, and it is generally accepted that peculiar magnetic fields support them against the pull of gravity and insulate them from the heat of the corona (Rust & Kumar 1994; Hirayama 1979, 1985; Poland 1986; Priest 1989; Ruzdjak & Tandberg-Hanssen 1990).
Prominences are filaments seen at the solar limb, but they are seen in
two-dimensions, and can be more usefully studied. Whether
prominences
or filaments, they have many unknowns: source of
the material, formation etc., and further investigation is necessary.
On 29 August 1990, we observed an eruptive prominence, and a series of
filtergrams and 
spectra were obtained. In
this paper,
the prominence will be studied to reveal its structure, evolution and
kinematic
characteristics in detail.