Closed magnetic structures in the chromosphere and in the transition region

Using simultaneous observations of the same solar regions in the lines H-alpha and C IV 1548 A, schematic models of closed magnetic lines have been derived from dynamical constraints. It is concluded that the magnetic loops are closed at higher levels above facular than above nonfacular regions. This result remains valid whatever are the assumed density models and even if the 3-min oscillations are taken into account. The center-to-limb behavior is well predicted by taking into account the relative opacity in the chromosphere and transition region.