3-D magnetic configurations supporting prominences - III. Evolution of fine structures observed in a filament channel

On September 25th 1996, a quiescent filament located near the center disc ( S2, E5) was observed on the German VTT (Tenerife) with the MSDP instrument, in the H alpha line center and wings. SOHO/MDI line-of-sight magnetograms were co-aligned with the MSDP images, showing the position and evolution of the lateral feet of the filament in the vicinity of the parasitic magnetic polarities observed in the filament channel. Using the assumptions developed in the previous papers of this series relat ed to the reconstruction of the 3-D magnetic configuration of filaments, we perform "linear magnetohydrostatic" extrapolations (taking into account th e effects of plasma pressure and gravity) on the SOHO/MDI magnetograms. The main hypothesis is the presence of a twisted flux-tube located above the p hotospheric inversion line. Assuming that the parameters of the model do not need to be significantly m odified during the evolution of the configuration for a duration of 1 day, we have shown that the 3-D distribution of dipped field lines is well corre lated with H alpha<INF></INF> dark absorbing features in the filament chann el: the filament itself, its lateral feet and some of the surrounding dark fibrils. In this way we confirm what was suggested in our earlier papers, i .e. that the feet are composed of the dipped portions of some held lines, w hich form a continuous pattern from the corona to the photosphere. We propo se the same explanation for the magnetic configuration of some of the dark H alpha fibrils in the channel. We show that the plasma effects are not res ponsible for the existence of most of the magnetic dips, however their incl usion helps to get a better correspondence between the model and the observ ations. We find that the average H alpha Doppler velocities associated with the filament and with the chromospheric fibrils is of the order of a few h undred m s<SUP>-1</SUP> (though it can go locally up to 3 km s<SUP>-1</SUP> in the filament). These upward velocities are consistent with a quasi-stat ic evolution of the magnetic configuration and with the support of dense pl asma in magnetic dips.