Solar rotation plays an important role in the conversion of transverse and longitudinal magnetic fields, and is a key basis for revealing the origin and evolution of solar magnetic fields, but the long-term evolution of coronal rotation has not been fully understood. The intensity of coronal green line radiation from January 1, 1939 to December 31, 2023 is studied using ensemble empirical mode decomposition and wavelet analysis. The findings include: (1) The significant periods of the coronal Fe XIV green line radiant intensity are 15.64 d, 27.99 d, 70.37 d, 162.79 d, 314.50 d, 1.89 yr, 10.30 yr and 11.04 yr, and the first three periods are closely related to the coronal rotation. (2) During the 18—24 solar activity cycle, the period length of coronal rotation shows a downward trend, that is, the coronal rotation speed is constantly accelerating. (3) The period length of coronal rotation is closely related to Rieger period, quasi-biennial oscillation and quasi-six-year oscillation.