Аннотация:The brightness of the solar corona as a whole (limb+disk) in the green line (Fe XIV 5303 Å) is estimated from the database created by J. Sykora. This coronal index GLS (Green Line Sun) is based on observations directly. A daily set of from 1939 to 2001 is analyzed with the adaptive wavelet techniques. The method applied for the Sun is the same as it used for late-type stars. We found that the synodic rotational period for inhomogeneities in the corona can exceed the mean value up to 3-4 days during epochs of the high activity. Hence it appears that ∆Ω/<Ω> = -0.13. The slowest rotation occurs when the sign of the global magnetic dipole of the Sun changes.