We report on the parallel analysis of the periodic behaviour of coronal mass
ejections (CMEs) based on 21 years [1996 -- 2016] of observations with the
SOHO/LASCO--C2 coronagraph, solar flares, prominences, and several proxies of
solar activity. We consider values of the rates globally and whenever possible,
distinguish solar hemispheres and solar cycles 23 and 24. Periodicities are
investigated using both frequency (periodogram) and time-frequency (wavelet)
analysis. We find that these different processes, in addition to following the
≈11-year Solar Cycle, exhibit diverse statistically significant
oscillations with properties common to all solar, coronal, and heliospheric
processes: variable periodicity, intermittence, asymmetric development in the
northern and southern solar hemispheres, and largest amplitudes during the
maximum phase of solar cycles, being more pronounced during solar cycle 23 than
the weaker cycle 24. However, our analysis reveals an extremely complex and
diverse situation. For instance, there exists very limited commonality for
periods of less than one year. The few exceptions are the periods of 3.1--3.2
months found in the global occurrence rates of CMEs and in the sunspot area
(SSA) and those of 5.9--6.1 months found in the northern hemisphere. Mid-range
periods of ≈1 and ≈2 years are more wide spread among the
studied processes, but exhibit a very distinct behaviour with the first one
being present only in the northern hemisphere and the second one only in the
southern hemisphere. These periodic behaviours likely results from the
complexity of the underlying physical processes, prominently the emergence of
magnetic flux.Comment: 33 pages, 15 figures, 2 table