Turbulent motions and magnetic fields are a key component of coronal heating mechanisms. They are indeed likely to produce the small scales at which the mechanisms such as reconnection are efficient enough. The properties of turbulence (and the associated intermittency) may thus have an influence on the energy dissipation in the corona, and need to be characterized from observations. Although turbulence is omnipresent from the Sun to the heliosphere, good observations of MHD turbulence have not yet been performed in the corona, in lines emitted at high temperature, where the heating actually occurs. We propose a study of coordinated EUSEUI-VIM observations, with better resolution and counting statistics than ever before, whose main goal is to get and interpret the spatial statistics (spectra and structure functions) of the velocity field in lines emitted at high temperatures (log_10 T≥6.4), together with the plasma and magnetic environment of the observed region. These statistics will help us understand the precise role of coronal turbulence in the coronal heating processes.
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