Stephan Zidowitz
Due to the rotation of the sun, the solar corona can be observed under different directions at different times. Using methods of computer tomography the underlying three-dimensional structure can be reconstructed from the observed projection data. For the 'Whole Sun Month', August 10 - September 8, 1996, we present here reconstructions of the inner part of the corona. From images of the green Fe XIV line taken with the LASCO-C1 Coronagraph we reconstruct the emission density and from images of the Mark III K-coronameter of the Mauna Loa Solar Observatory on Hawaii we reconstruct the destribution of the electron density. Further we compare the achieved structures with global 'potential-field' models of the solar magnetic field based on the photospheric data from the Wilcox Solar Observatory.