Core Bounce Density in Massive Progenitors Compared with the Torsion Density Ceiling

The central density reached at core bounce is the closest any stellar explosion comes to the densities at which spin-torsion corrections could matter. Published collapse calculations place bounce densities near nuclear saturation, yet the neutron-carrier torsion ceiling lies near 10^55 g per cubic centimetre. This paper asks how large the separation is across the progenitor mass range and whether any plausible equation-of-state variation could close it. Using the calculation described in the Methods, the headline results are: rhoA_g_cm3 = 9.72e+54, rho_max_g_cm3 = 6.1e+14, margin_min_orders = 40.2, margin_12Msun_orders = 40.5. Even the densest case in the grid remains more than forty orders of magnitude below the ceiling. Rotation and a softer equation of state move the bounce density by factors of order unity, not by decades, so the conclusion is insensitive to the modelling choices examined. Core bounce in ordinary supernovae therefore does not probe the torsion ceiling directly; its relevance is as a consistency check, since any model predicting bounce near the ceiling would already contradict the observed explosion population. This study is simulated and computed from stated assumptions; it is not a measurement. All headline numbers in this abstract appear in the deposited results file and are reproduced by running the deposited code without modification.