Abstract Different processes involving the magnetic field and its fine structures in the atmosphere have been proposed to explain the heating of the corona. To help explore phenomena related to these different processes, we will report some new observations of oscillations in fine chromospheric structures using the MSDP spectrograph operating at Meudon and the UVSP spectrograph aboard SMM. The temporal analysis of radial velocities measured in the C IV line shows that no oscillations are detectable in the transition zone. It is in good agreement with the wave reflection model generally admitted. In the Hα line the 2 D analysis points out that the energy observed in an unresolved frequency range around 250 s in the chromospheric power spectrum is in fact concentrated in structures parallel to chromospheric fibrils along which the phase extends coherently. The oscillations appear to be transverse and might be interpreted either by Alfv́en waves generated in the chromosphere and propagating through magnetic filamentary structures or by eigenmodes of filamentary structures excited by chromospheric p-modes.
Oscillations detected in C IV and Hα lines in magnetic structures
Advances in Space Research ; 11 , 4 ; 195-198
1991-01-01
4 pages
Article (Journal)
Electronic Resource
English
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