Abstract Using advanced processing techniques, we analyze high-cadence, high-resolution extreme-ultraviolet images and show that, throughout the solar cycle, midlatitude coronal holes (CHs) are made up of ubiquitous and space-filling funnel-shaped structures (or cells) anchored to unipolar magnetic flux concentrations in network lanes. We demonstrate that the coronal cells, previously documented in the magnetically closed regions, and coronal plumes, inside CHs, are a particular manifestation of ubiquitous cells. The cell properties depend on the magnetic field intensity at their footpoint and connectivity in the corona, either closing in opposite-polarity regions (CF-cells) or extending to form open field (OF-cells). The OF-cells reach size scales on the order of supergranules and are characterized by dark lanes delimiting ray-like features both showing, at different levels, persistent jetlike ejections. The cells’ lifetime mirrors that of magnetic flux concentrations revealed by magnetograms, slowly emerging and then disappearing in a matter of a few hours to a few days in a one-to-one correspondence. When a cell forms along the CH boundary, it can alter the CH boundary by shrinking or expanding the CH by an approximately supergranular cell unit. Therefore, coronal cells can contribute to the dynamics of the CH boundary. We contextualize these observations in a “coronal cell” theory potentially able to provide an explanation for fine-scale coronal structures and jetting activity in polar CHs.
