Abstract
Based on the developed method of jointly using data on the magnetic fields and brightness of fila- ments and coronal holes (CHs) at various heights in the solar atmosphere as well as on the velocities in the photosphere, we have obtained the following results: —The upward motion of matter is typical of filament channels in the form of bright stripes that often surround the filaments when observed in the HeI 1083 nm line. —The filament channels observed simultaneously in H α and HeI 1083 nm differ in size, emission characteris- tics, and other parameters. We conclude that by simultaneously investigating the filament channels in two spec- tral ranges, we can make progress in understanding the physics of their formation and evolution. —Most of the filaments observed in the HeI 1083 nm line consist of dark knots with different velocity distri- butions in them. A possible interpretation of these knots is offered. —The height of the small-scale magnetic field distribution near the individual dark knots of filaments in the solar atmosphere varies between 3000 and 20000 km. —The zero surface separating the large-scale magnetic field structures in the corona and calculated in the poten- tial approximation changes the inclination to the solar surface with height and is displaced in one or two days. —The observed formation of a filament in a CH was accompanied by a significant magnetic field variation in the CH region at heights from 0 to 30000 km up to the change of the predominant field sign over the entire CH area. We assume that this occurs at the stage of CH disappearance. DOI: 10.3103/S0190271708010105
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