This arXiv preprint (not yet peer-reviewed) uses two independent simulation suites—Marvelous Massive Dwarfs/Marvel-ous Dwarfs and FIRE-2—to quantify a systematic shortfall in OVI absorption within the circumgalactic medium of dwarf galaxies. The authors track oxygen mass produced across each galaxy’s star-formation history and compare it against observed column densities, finding underproduction plus inefficient transport to large radii. Methodology relies on ~dozens of zoom-in runs spanning different codes and feedback implementations; sample limitations include idealized UV backgrounds and resolution floors that still leave subgrid metal mixing unresolved. Prior COS-Halos and COS-Dwarfs observations (Tumlinson et al. 2011; Johnson et al. 2017) established extended OVI reservoirs at log N_OVI ~14, yet both simulation families self-select only cool, low-density, modestly enriched gas. The work correctly flags supernova yield assumptions and metal-loading factors in low-metallicity regimes as likely culprits—points earlier EAGLE and IllustrisTNG analyses (Schaye et al. 2015; Pillepich et al. 2018) touched on but did not isolate for dwarfs. What prior coverage missed is the direct mass-budget test linking missing OVI to cumulative metal ejection efficiency rather than ionization alone. Until subgrid prescriptions improve metal dispersal without over-heating the CGM, the “SOS” problem will persist across next-generation runs.