The physics of the solar atmosphere is complex from both theoretical and modeling perspectives. The plasma temperature from the photosphere to the corona increases from ~5,000 K to ~1 million K over a distance of only ~10,000 km from the chromosphere and the transition region. How can the corona heat up to millions of degrees K? How do the coronal plasma and magnetic field interact with each other? These fundamental questions of solar physics are gaining more and more attention as NASA's Parker Solar Probe mission is coming closer to exploring the solar corona. Studies of coronal heating focus on closed loop regions, open magnetic field regions and global corona. These regions are involved in physical processes such as magnetic reconnection and turbulence thought to be responsible for heating the solar corona. This session welcomes theoretical, numerical simulation, and observational contributions on the developments of physics of solar coronal heating.