QUIET-SUN CONNECTION BETWEEN THE C-IV RESONANCE LINES AND THE PHOTOSPHERIC MAGNETIC-FIELD

The quiet-Sun relation between the C IV resonance line parameters and the photospheric magnetic field is studied with a spatial resolution o f 1'' x 1''. The material is ordered into groups according to the magn itude of the magnetic flux density, \B\, and conditional probabilities are calculated. We find that redshifted profiles with either high int ensity, large Doppler shift, or large line broadening occupy an increa sing fraction of the area when \B\ increases. These results are contra sted by blueshifted profiles which indicate a slight decrease with inc reasing magnetic flux density. The similarity in the results obtained with magnetograms taken several hours before and after the UV data led us to suggest that the tendency for redshifted profiles to outnumber blueshifted profiles in quiet regions originates in the supergranular network. Suggestions regarding the origin of the redshift phenomenon a re briefly confronted with the observations. It appears difficult to e xplain the observations with models based on continuous gas flows. How ever, a model containing Alfven wave pulses traveling from the corona toward the transition region promises to be compatible with the observ ations.