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The quiet Sun (QS) harbors a tremendous amount of magnetic flux, comparable to what is found in active regions during the maximum of the solar cycle. This flux is distributed between network (NE) and internetwork (IN) magnetic features. The former surrounds the supergranular cells, while the latter fills up the cell interiors. Together, NE and IN create a highly dynamic environment in which magnetic fields frequently emerge on the solar surface, constantly move and interact with each other. These interactions and the rise of IN loops through the solar atmosphere may significantly support chromospheric heating, while the IN fields dragged by convective flows toward the boundaries of supergranules maintain the NE. QS fields are so abundant that understanding their properties and role in solar magnetism is crucial to our understanding of how the Sun generates its magnetic fields and heats its atmosphere. In this talk, I will discuss our latest results and knowledge of the Sun’s quiet magnetic fields, including their possible origin, spatiotemporal evolution, and how they affect the dynamics and energetics of the solar atmosphere.

Watch the recording.