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MHD waves are ubiquitous in the solar corona where the highly structuredmagnetic fields provide efficient wave guides for their propagation. While MHDwaves have been observed originating from lower layers of the solar atmosphere,recent studies have shown that some can be generated in-situ by the collisionof dense counter propagating flows. In this theoretical study, we analyse themechanism that triggers the propagation of kink and sausage modes in the solarcorona, following the collision of counter-propagating flows and how theproperties of the flows affect the properties of the generated waves. In orderto study in detail such a mechanism we run a series of ideal 2D and 3D MHDsimulations where we vary the properties of the counter-propagating flows andby means of a simple technique to estimate the amplitudes of the kink andsausage modes, we investigate their role on the generation and propagation ofthe MHD waves. We find that the amplitude of the waves is largely dependent onthe kinetic energy of the flows and that the onset of kink or sausage modesdepends on the asymmetries between the colliding blobs. Moreover, the initialwavelength of the MHD waves is associated with the magnetic configurationresulting from the collision of the flows. We also find that genuine 3D systemsrespond with smaller wave amplitudes. In this study, we present a parameterspace description of the mechanism that leads to the generation of MHD wavesfrom the collision of flows in the corona. Future observations of these wavescan be used to understand the properties of the plasma and magnetic field ofthe solar corona.

MHD simulations of the in-situ generation of kink and sausage waves in the solar corona by collision of dense plasma clumps