The Magellanic (SMC–LMC) Bridge is a narrow, clumpy stream of neutral gas and stars physically linking the Small and Large Magellanic Clouds, with evidence for in-situ star formation, chemically inhomogeneous gas, and multiple tidal episodes over gigayear timescales (Grebel et al. 1999; Rolleston et al. 1999). While ΛCDM can attribute such a bridge to tidal and ram-pressure interactions during close passages, reproducing simultaneously the detailed morphology, metallicity pattern, longevity, and the tightly bound, near–first-infall SMC–LMC–Milky Way configuration in simulations is non-trivial, making the observed Bridge and its dynamical context a sensitive small-scale challenge for standard models (Besla et al. 2010; Nidever et al. 2013).