Black bounces as magnetically charged phantom regular black holes in Einstein-nonlinear electrodynamics gravity coupled to a self-interacting scalar field

As previously proposed in Simpson and Visser [J. Cosmol. Astropart. Phys. 02 (2019) 042], Mazza et al. [J. Cosmol. Astropart. Phys. 04 (2021) 082], Franzin et al. [J. Cosmol. Astropart. Phys. 07 (2021) 036], and Lobo et al. [Phys. Rev. D 103, 084052 (2021), the "black bounce" spacetimes are an interesting type of globally regular modifications of the ordinary black holes (such as the Kerr-Newman geometry and its particular cases) which generically contain a spacetime singularity (usually of the curvature type) at their center. To transforms a static, spherically symmetric and asymptotically flat black hole (SSS-AF-BH) geometry regular everywhere except its center of symmetry r 1/4 0 (where r stands for the "areal radius" of the two-dimensional spheres of symmetry) and with (outer) event horizon at r 1/4 rh > 0, into a black pffiffiffiffiffiffiffiffiffiffiffiffiffiffibounce spacetime, is to simply replace r with rho 2 thorn a2 and dr with d rho, being rho a new radial coordinate, pffiffiffiffiffiffiffiffiffiffiffiffiffiffiand a is some real constant nonzero. As long as rh 1/4 rho 2 h thorn a2 > jaj, the result is a globally regular (or singularity-free) black hole spacetime (called black bounce) where the singularity that occurs in the ordinary SSS-AF-BH geometry at r 1/4 0 now in the transformed geometry turns into a regular spacetime region determined by the two-dimensional spheres of symmetry of radius jaj, while the areal radius pffiffiffiffiffiffiffiffiffiffiffiffiffiffi rho 2 thorn a2 always remains positive for all rho is an element of o-infinity; infinity thorn and has a minimum at rho 1/4 0 given by jaj. Hence, in the transformed spacetime, the areal radius has a minimum, decreasing before and increasing after this minimum (defining two SSS-AF regions that bounce). In this work we will present several black-bounces exact solutions of General Relativity. Among them is a novel type of black-bounce solution, which contrast to the Simpson-Visser type {[Simpson and Visser, J. Cosmol. Astropart. Phys. 02 (2019) 042], [Mazza et al., J. Cosmol. Astropart. Phys. 04 (2021) 082], [Franzin et al., J. Cosmol. Astropart. Phys. 07 (2021) 036], [Lobo et al., Phys. Rev. D 103, 084052 (2021)]}, does not have the Ellis wormhole metric as particular case. The source of these solutions is linear superposition of phantom scalar fields and nonlinear fields.