tokens: closer, due to an attractive Lorentz force, in the same way as in CsTsB above. The loops then merge and seem to cross each other, because the positive toroidal field of the loop located at lower latitudes ends up appearing at higher latitudes at t = 4 days and later. From the temporal evolution of the energies that were shown in Figure 6 , it is clear that this case is the one producing the largest release of magnetic energy—because of the multiple reconnections—and thus the largest increase in kinetic energy. However, the loops do not seem to fully reconnect; the two main initial structures are still visible after eight days of evolution. However, it is still clear that the loops underwent a strong loss of magnetic intensity. Indeed, after four days, only 30% of the initial magnetic intensity remains in the loops, and only 20% remains after 5.4 days. As we shall see in the next section, even if the magnetic structures still seem to be well-confined in latitude and radius, the morphology of the emerging radial field is very different from the other cases. Figure 14. Same as Figure 7 , but for CoToBw. In this case, a strong interaction occurs between the structures: the loop of positive B φ passes through the loop of negative B φ after three to four days of evolution. 4. Consequences for Emerging Regions One of the main motivations to study interacting Ω-loops was to investigate the consequences of such interactions on emerging magnetic regions at the solar surface. We note here that, in our calculations, the top of the domain is located at r = 0.96 R ⊙ , i.e., still quite far from the solar surface—but we can get some insight on the possible implication for solar active regions by looking at the radial magnetic field close to the top of our domain in each case. In this section, we begin by focusing on the top panels of Figures 15 – 19 ; we will discuss the bottom panels (mainly the radial current maps) in the next section. Figure 15. Case CoTsBw. Top panel: zoom on the emerging radial magnetic field at r = 0.93 R ⊙ at three different times. Bottom panel: sketch of the initial configuration, with an emerging radial field at r = 0.93 R ⊙ shown on the whole Northern hemisphere and a zoomed map of the radial current J r at the last time t = 10 days. On this last panel, we superimpose contours of the radial magnetic field at 80% (thicker) and 2% (thinner) of its min and max values. The PIL, indicated by the magenta arrows, is then visible when the contours at 2% of opposite sign meet. Two emerging regions of different handedness are clearly visible here. Figure 16. Same as Figure 15 , but for case CsTsB. The black arrows on the bottom mid-panel indicate the locations of strong magnetic “necklaces.” In this merging case, the emerging radial field mostly consists of one large bipolar structure. Figure 17. Same as Figure 15 , but for case CsTsBw. In this weaker field case, the magnetic structure has been more affected by convective motions, and the
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