  Macrospicules (MS) are localised small-scale jet-like phenomena in the solar
atmosphere, which have the potential to transport considerable amount of
momentum and energy from the lower solar atmospheric regions to the Transition
Region and the low corona. A detailed statistical analysis of their temporal
behaviour and spatial properties is carried out in this work. By means of
state-of-the-art spatial and temporal resolution observations, yielded by the
Atmospheric Imaging Assembly (AIA) of Solar Dynamics Observatory (SDO), we
constructed a database covering a 5.5-year long period, containing 301
macrospicules that occurred between June 2010 and December 2015 detected at
30.4 nm wavelength. Here, we report the long-term variation of the height,
length, average speed and width of MS in Coronal Holes and Quiet Sun areas both
in the northern and southern hemisphere of the Sun. This new database helps to
refine our knowledge about the physical properties of MS. Cross-correlation of
these properties show a relatively strong correlation, but not always a
dominant one. However, a more detailed analysis indicates a wave-like signature
in the behaviour of MS properties in time. The period of these long-term
oscillatory behaviours are just under two years. Also, in terms of solar
north/south hemispheres, a strong asymmetry was found in the spatial
distribution of MS properties, which may be accounted for the solar dynamo.
This latter feature may then indicate a strong and rather intrinsic link
between global internal and local atmospheric phenomena in the Sun.
