Solar coronal activity and evolution of the magnetic field

We discuss the role of the solar magnetic field in forming of stable activity structures during the current solar cycle 23. These structures are clustered in long-liver complexes of activity in the photosphere and are visible in the transition region and corona in an extreme ultraviolet irradiance as bright loops. We have represented the EUV data from SOHO/EIT in four wavelengths (171, 195, 284 and 304) in the form of coronal synoptic maps for 1996-2000. The distributions of intensity of the coronal lines are related to magnetic activity and show non-uniform distributions as a function of Carrington longitude and latitude. In the axisymmetrical case we have detected two waves of coronal, activity in both hemispheres. The first, equatorward wave, is connected with complexes of sunspot activity. The second, polarward wave, reflects the giant loops structures which connect regions of polar magnetic field with the following parts of complexes of solar activity, and, probably, plays important role in the topological evolution of the solar magnetic field.