The solar corona and inner heliosphere provide a natural laboratory to understand how magnetized plasmas are heated, accelerated and structured over a wide range of temporal and spatial scales. This session explores the many facets of physical processes involved in coronal heating and solar wind acceleration; in the origins of different solar wind streams, from the fastest, to the Alfvénic slow, to the typical slow and to the sub-Alfvénic winds seen inside 10 Rs by Parker Solar Probe. What is the magnetic switchback’s role in accelerating the wind? How does source magnetic topology in the solar atmosphere determine different wind properties? How coronal and solar wind structures change when moving from chaotic solar maximum to orderly solar minimum and what can we learn about the inner heliosphere from this transition? 

This session, currently in its 13^th year, solicits contributions on all fundamental aspects of coronal and inner heliosphere plasma physics.