  MHD waves are ubiquitous in the solar corona where the highly structured
magnetic fields provide efficient wave guides for their propagation. While MHD
waves have been observed originating from lower layers of the solar atmosphere,
recent studies have shown that some can be generated in-situ by the collision
of dense counter propagating flows. In this theoretical study, we analyse the
mechanism that triggers the propagation of kink and sausage modes in the solar
corona, following the collision of counter-propagating flows and how the
properties of the flows affect the properties of the generated waves. In order
to study in detail such a mechanism we run a series of ideal 2D and 3D MHD
simulations where we vary the properties of the counter-propagating flows and
by means of a simple technique to estimate the amplitudes of the kink and
sausage modes, we investigate their role on the generation and propagation of
the MHD waves. We find that the amplitude of the waves is largely dependent on
the kinetic energy of the flows and that the onset of kink or sausage modes
depends on the asymmetries between the colliding blobs. Moreover, the initial
wavelength of the MHD waves is associated with the magnetic configuration
resulting from the collision of the flows. We also find that genuine 3D systems
respond with smaller wave amplitudes. In this study, we present a parameter
space description of the mechanism that leads to the generation of MHD waves
from the collision of flows in the corona. Future observations of these waves
can be used to understand the properties of the plasma and magnetic field of
the solar corona.
