The two-fold outcome of the action can be summarized as (1) there often exists a complex magnetic topology at the feet of coronal loops, and (2) footpoint magnetic reconnection is the likely source of energy to heat the corona. These findings advance our understanding of the physics of the solar atmosphere. It was generally assumed that coronal loops are connected to a pair of opposite-polarity magnetic field patches on the solar surface. In this scenario, each footpoint is represented by a simple configuration of unipolar magnetic field in the photosphere. Contrary to this common view, our high-spatial resolution observations of the solar photosphere revealed that coronal loops are often rooted in regions with complex magnetic topology. At one or both the footpoints, the unipolar magnetic field patch that can extend to several megameters on the solar surface, is observed to be surrounded by small-scale (a few 100 km) magnetic field features with polarity that is opposite to that of the main patch. Models that focus on the photosphere-corona coupling will benefit from the new details on the complex magnetic field structure at the feet of coronal loops identified through this action. The second part of the action’s outcome deals with coronal heating. In traditional view, coronal heating is facilitated by the horizontal motions of magnetic field in the solar photosphere. These motions launch MHD waves into the solar atmosphere or stress and braid the coronal magnetic field. The energy associated with these waves or braids is then dissipated in the corona to heat the plasma. Although models based on waves and braids have been well studied, the dominant role of either of these processes in heating the corona, is not well established. Our findings highlight the key role of the complexity of the photospheric magnetic field and its interaction between small-scale opposite polarities in heating the solar corona. Based on these results, we point to a specific way, namely, magnetic reconnection due to flux emergence and cancellation at the feet of coronal loops, as a conduit of mass and energy into the corona. The action led to the proposal of a new mechanism of coronal heating through flux cancellation. Our results are expected to motivate further studies in the future to decipher the puzzle of coronal heating in cool-stars like the Sun. Observations of flux emergence and cancellation at the feet of coronal loops with upcoming solar telescopes, capable of resolving the Sun down to 30 km, will improve our understanding of the magnetic reconnection, a fundamental process in the universe.