  Determining the mechanisms responsible for the heating of the coronal plasma
and maintaining and accelerating the solar wind are long standing goals in
solar physics. There is a clear need to constrain the energy, mass and momentum
flux through the solar corona and advance our knowledge of the physical process
contributing to these fluxes. Furthermore, the accurate forecasting of Space
Weather conditions at the near-Earth environment and, more generally, the
plasma conditions of the solar wind throughout the heliosphere, require
detailed knowledge of these fluxes in the near-Sun corona. Here we present a
short case for a space-based imaging-spectrometer coronagraph, which will have
the ability to provide synoptic information on the coronal environment and
provide strict constraints on the mass, energy, and momentum flux through the
corona. The instrument would ideally achieve cadences of $\sim10$~s, spatial
resolution of 1" and observe the corona out to 2~$R_{\sun}$. Such an instrument
will enable significant progress in our understanding of MHD waves throughout
complex plasmas, as well as potentially providing routine data products to aid
Space Weather forecasting.
