The Neutrino Burst from a Bounced Core: What the Density Cap Does to the Signal of a Core That Would Have Formed a Black Hole

In the Einstein-Cartan spin-torsion frame defined by the Aldred Limit, rho_A = 9.72e54 g/cm^3, collapse halts at the density cap and bounces; on the branch where collapse continues past nuclear density, no black hole forms. This paper prices the consequence for the neutrino signal of the next galactic core-collapse event, against the standard failed channel in which the proto-neutron star accretes past its maximum mass, forms a black hole, and the neutrino signal (total ~3e53 erg) is cut off abruptly. In the frame the cutoff is replaced by a bounce pulse carrying a fraction eps_b of the core's 1e53 erg binding-energy scale. With a stated detector model, at 10 kpc and eps_b = 0.1 the pulse gives a 10 ms window excess of 374 events in Super-Kamiokande, 3,109 in Hyper-Kamiokande, 315 in JUNO and 287 in DUNE (93-291 sigma). A 5-sigma discrimination at 10 kpc requires eps_b >= 1.7e-3 (Hyper-Kamiokande) to 5.4e-3 (JUNO); at eps_b = 1e-2 all four detectors reach 5 sigma across the Galaxy (18-58 kpc). Negative result at full size: if only the mass that reaches the cap radiates (1.67e13 to 4.17e24 g from companion first-touch computations), eps_b <= 3.8e-8 and the excess is 1.4e-4 events -- the bounce is undetectable in neutrinos. The test decides only for eps_b >= ~2e-3, and on the successful-supernova branch the frame's signal is identical to the standard signal (Delta rho/rho ~ 3.1e-41). All numbers are model calculations from the deposited script (compute.py): SIMULATED, NOT MEASURED. AI-use disclosure: Drafted with the assistance of Dave, an AI research system; all computations are reproducible from the included script.