  Coronal and interplanetary shock waves produced by coronal mass ejections
(CMEs) are major drivers of space-weather phenomena, inducing major changes in
the heliospheric radiation environment and directly perturbing the near-Earth
environment, including its magnetosphere. A better understanding of how these
shock waves evolve from the corona to the interplanetary medium can therefore
contribute to improving nowcasting and forecasting of space weather. Early
warnings from these shock waves can come from radio measurements as well as
coronagraphic observations that can be exploited to characterise the dynamical
evolution of these structures. Our aim is to analyse the geometrical and
kinematic properties of 32 CME shock waves derived from multi-point white-light
and ultraviolet imagery taken by the Solar Dynamics Observatory (SDO), Solar
and Heliospheric Observatory (SoHO), and Solar-Terrestrial Relations
Observatory (STEREO) to improve our understanding of how shock waves evolve in
3D during the eruption of a CME. We use our catalogue to search for relations
between the shock wave's kinematic properties and the flaring activity
associated with the underlying genesis of the CME piston. Past studies have
shown that shock waves observed from multiple vantage points can be aptly
reproduced geometrically by simple ellipsoids. The catalogue of reconstructed
shock waves provides the time-dependent evolution of these ellipsoidal
parameters. From these parameters, we deduced the lateral and radial expansion
speeds of the shocks evolving over time. We compared these kinematic properties
with those obtained from a single viewpoint by SoHO in order to evaluate
projection effects. Finally, we examined the relationships between the shock
wave and the associated flare when the latter was observed on the disc by
considering the measurements of soft and hard X-rays.
