Page tree

Versions Compared


  • This line was added.
  • This line was removed.
  • Formatting was changed.


◦       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.