Speckle interferometric techniques can greatly improve the spatial resolution of solar observations. By applying this technique to polarimetric observations in the wing of a Zeeman-sensitive spectral line, a few magnetic fluxtubes have been resolved in the past. I, using the Universal Birefringent Filter with a bandwidth of 25 pm in the Ca I line at 610.3 nm. Bruce Wilton, an NSO summer student supervised by Keller, has analyzed more than 60 regions in the quiet network. The figure shows one of the areas where the size, brightness, flux, and dynamics of fluxtubes are determined, which is essential to reach an understanding of important solar phenomena such as chromospheric and coronal heating, irradiance variations, magnetic dynamos, and stellar activity in general.
Preliminary results indicate that the larger elements are barely resolved.
Most magnetic elements in the network seem to be brighter than the average intensity in white light at disk center, in contrast to the dark structures seen in plages at disk center. A small region in the quiet network close to solar disk center. The graphs on the bottom correspond to cuts across the images as indicated by the white and black lines in the images at the top. The intensity structures in the line wing are comparable to images obtained in the G band. In the magnetogram, grey corresponds to no magnetic signal.