The Aldred Limit Inside a Neutron Star: A Computed Absence and What It Excludes

If the Aldred Limit is correct, its effects inside a neutron star are computable, and this paper computes them: at five times nuclear saturation density, near the top of the plausible range for neutron star centres, the Einstein-Cartan spin-torsion correction to the effective density is a fraction 1.44e-40 of the density itself. The correction reaches one part in a million only at 9.72e+48 g per cubic centimetre and one percent only at 9.72e+52 g per cubic centimetre. The gap between the densest neutron star centres and the Limit is a factor 6.94e+39. The conclusion is plainly negative for one common hope: no observation of neutron star masses, radii, or cooling can test the neutron-branch Limit, because its predicted effects there are dozens of orders of magnitude below any conceivable measurement precision. Conversely, the framework is not embarrassed by the success of torsion-free neutron star modelling; it predicts that success. Tests of the Limit must look to the early universe or to collapse itself. Computed from stated assumptions, not measured.