Authors: Milan Gosic (LMSAL/BAERI)

The quiet regions of the solar surface are densely populated with small and weak flux patches. They contain an amount of magnetic flux comparable to what is found in active regions during the peak of the solar cycle. Because of this, it is believed that these small-scale fields are essential ingredients of the solar magnetism and may play a pivotal role in mass and energy transport through the solar atmosphere. The quiet Sun (QS) flux is distributed between network (NE) and internetwork (IN) magnetic features. IN fields populate the interior of supergranular cells, while the NE outlines the boundaries of supergranules. Together, they create a dynamic environment where magnetic fields frequently emerge, move, and interact with each other. The spatiotemporal evolution of the QS magnetic fields is coupled to convective motions and leads to generation of various processes that may contribute to chromospheric heating, such as vortices, emergence and reconnection of magnetic field lines, generation of MHD waves, etc. In this talk, I will review our current understanding of the QS magnetic activity and how it impacts the energetics and dynamics of the quiet solar atmosphere.