In general:


◦       Determine the properties of the coronal plasma sources and their evolution during the wind acceleration from the photosphere to the corona.

◦       Identify the physical processes responsible for the evolution of the boundaries between wind types (shocks, shears, reconnection).

◦       Track the spatial evolution of the interfaces between fast, intermediate, and slow solar wind regimes at the solar surface and in the inner and extended corona.

◦       Determine the relative roles of coronal source effects and interplanetary processing in the appearance of the heliospheric plasma at 1 AU (radial evolution).

◦       Characterise turbulence/fluctuations and link to processes at work in source regions.

◦       Measure the variability of the solar wind outflow velocity mapped over the full outer corona through the solar cycle.


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