  Jets, whatever small (e.g. spicules) or large (e.g. macrospicules) their
size, may play a key role in momentum and energy transport from photosphere to
chromosphere and at least to the low corona. Here, we investigate the
properties of abundant, large-scale dynamic jets observable in the solar
atmosphere: the macrospicules (MS). These jets are observationally more
distinct phenomena than their little, and perhaps more ubiquitous, cousins, the
spicules. Investigation of long-term variation of the properties of
macrospicules may help to a better understanding of their underlying physics of
generation and role in coronal heating. Taking advantage of the high temporal
and spatial resolution of the Solar Dynamics Observatory, a new dataset, with
several hundreds of macrospicules, was constructed encompassing a period of
observations over six years. Here, we analyse the measured properties and
relations between these properties of macrospicules as function of time during
the observed time interval. We found that cross-correlations of several of
these macrospicule properties display a strong oscillatory pattern. Next,
wavelet analysis is used to provide more detailed information about the
temporal behaviour of the various properties of MS. For coronal hole
macrospicules, a significant peak is found at around 2-year period. This peak
also exists partially or is shifted to longer period, in the case of quiet Sun
macrospicules. These observed findings may be rooted in the underlying
mechanism generating the solar magnetic field, i.e. the global solar dynamo.

Solar and Stellar Astrophysics