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E.E. Benevolenskaya (Pulkovo Observatory), A.G. Kosovichev, P.H. Scherrer (Stanford University)
We present the results of the investigation of the large-scale structure of the solar corona during the transition period between solar cycles 22 and 23 and at the beginning of the current cycle 23 using the SOHO/EIT EUV data obtained in 171Å, 195Å, 284Å~ and 304 Å~ lines. For this analysis the data were transformed into synoptic maps for each of the spectral lines, and for the 195Å/171Åline ratio which is an index of the coronal temperature. The synoptic maps reveal stable longitudinal structures in the coronal intensities and temperature, which are related to large-scale magnetic field structures. We discuss the relation between the coronal and photospheric magnetic structures obtained from the SOHO/MDI data, and compare the rotation rates of these structures with the rotation profile of the solar interior in order to determine the possible origin of the coronal structures.