||The heating of the solar chromosphere is a long-standing problem. Among all the mechanisms put forward to solve it, magnetohydrodynamic (MHD) waves and magnetic reconnection seem to be the most promising ones. However, they both invoke magnetic fields that are ubiquitously observed on the solar surface. Considering that most of the chromospheric heating occurs over the quiet Sun (QS), it is essential to understand how QS magnetic structures are coupled with the global heating of the solar atmosphere. The QS consists of network (NE) and internetwork (IN) regions. The former outlines the borders of supergranular cells, while the latter represents the cell interiors. Together, NE and IN represent a highly dynamical environment in which magnetic fields constantly emerge. Evolution of QS magnetic elements leads to generation of MHD waves, and numerous emergence and cancellation events that may significantly support chromospheric heating through magnetic reconnection. 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. I will discuss how the IRIS mission is helping us to understand the chromospheric heating, and what can we expect from the next generation telescopes in this regard.