The Large Magellanic Cloud (LMC) has a massive, rotationally supported, yet only moderately warped and thickened stellar–gaseous disk that has retained a coherent non-barred spiral arm and significant cold gas despite undergoing strong mutual tides with the Small Magellanic Cloud and now plunging into the Milky Way’s halo on a high-velocity, likely first-infall orbit (van der Marel 2004; Patel et al. 2020). In ΛCDM, repeated or even single close passages in a dense dark-matter environment, plus dynamical friction from the Milky Way’s and LMC’s dark halos, are expected to rapidly heat, strip, and disturb such a disk—often destroying long-lived spiral structure and producing more severe warps than observed—so keeping the LMC’s disk dynamically cold, gas-rich, and kinematically ordered over gigayear timescales demands fine-tuned halo masses, orbits, and feedback histories (Besla et al. 2012; Garavito-Camargo et al. 2019).