Microscopic and Macroscopic processes in the solar atmosphere and solar wind
Co-Convener: P. Hellinger 
Oral Programme
 / Mon, 20 Apr, 17:30–19:00  / Room 8
Poster Programme
 / Attendance Wed, 22 Apr, 17:30–19:00  / Halls X/Y

The magnetized atmosphere of our Sun is full of dynamic processes. Dynamic processes can trigger complex wave and turbulence activities in the corona and its extension -- the solar wind plasma. Waves and turbulence in the solar wind source regions on both microscopic and macroscopic scales are widely believed to play a key role in heating the corona and accelerating the solar wind plasma. The connection between the corona and the solar wind in interplanetary space can be viewed as the transition between a collision dominated region to a collision-free region. This session invites observational, theoretical, simulation and modelling studies that address plasma wave activities in the solar atmosphere and the solar wind. In particular, observational studies of wave and turbulence activities, coronal plasma parameters, plasma instabilities, multi-fluid and MHD modelling and kinetic simulations of the coronal and solar wind plasma are strongly encouraged.