- 1.1.1 Source regions of the fast solar wind
- 1.1.2 Source regions of the slow solar wind
- 220.127.116.11 Does slow wind originate from the over-expanded edges of coronal holes?
- 18.104.22.168 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes?
- 22.214.171.124 Abundance of minor ions as a function of height in the corona as indicator of slow or fast wind
- 126.96.36.199 Study of density fluctuations in the extended corona as a function of the outflow velocity of the solar wind while evolving in the heliosphere
- 188.8.131.52 Structure and evolution of streamers
- 184.108.40.206 Disentangle the spatial and temporal variability of the slow wind
- 220.127.116.11 Trace streamer blobs and other structures through the outer corona and the heliosphere.
- 18.104.22.168 Determine the velocity, acceleration profile and the mass of the transient slow wind flows
- 1.1.3 Source regions of the heliospheric magnetic field
- 22.214.171.124 Full characterization of photospheric magnetic fields and fine structures
- 126.96.36.199 How does the Sun's magnetic field link into space?
- 188.8.131.52 What is the distribution of the open magnetic flux?
- 1.1.4 Transverse themes
- 184.108.40.206 Reconnection
- 220.127.116.11.1 Interchange reconnection between open and closed field lines and its role in slow wind generation
- 18.104.22.168.2 Identify coronal reconnection sites by measuring impulsive event material
- 22.214.171.124.3 Identify reconnection exhausts in the solar wind
- 126.96.36.199.4 Current sheets inferred by determining the magnetic field geometries at local chromospheric heating sites
- 188.8.131.52.5 Identify and characterise the solar wind reconnection physics in current sheets with thickness down to the ion scales and smaller
- 184.108.40.206.6 Photospheric reconnection
- 220.127.116.11.7 Electron acceleration in coronal reconnection regions
- 18.104.22.168.8 Formation of flux ropes/CMEs via magnetic reconnection in the corona
- 22.214.171.124 Reconnection
◦ 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.