The arXiv preprint (v1, May 2026) from Griffiths et al. marks a methodological step forward by evolving two compact Wolf-Rayet progenitors—originally computed in 1D with GENEC and MESA—through the final minutes before collapse using the Aenus-Alcar 3D MHD code. With a sample of just two models, the work demonstrates that convective regions drive Reynolds stresses toward cylindrical rotation profiles approximating Ω ∝ ϖ^{-2}, while amplifying seed fields to near-equipartition toroidal-poloidal strengths with substantial small-scale power. This creates magnetic linkages across zones previously treated as disconnected in spherical 1D calculations. The preprint status means these findings await peer review, and the limited progenitor set restricts generality. When placed against earlier 2D axisymmetric studies (e.g., Mösta et al. 2015 on jet formation in rapidly rotating cores) and recent 3D neutrino-MHD simulations (e.g., Kuroda et al. 2020), the new results expose a critical gap: standard 1D angular-momentum transport prescriptions underestimate pre-collapse magnetic connectivity, potentially altering the topology that seeds neutron-star magnetic fields and the r-process yields that enrich galactic chemical evolution. The cylindrical redistribution also implies that core angular momentum may be more efficiently extracted than shellular assumptions predict, tightening the parameter space for magnetar versus ordinary pulsar birth channels.