Two-Solar-Mass Neutron Stars as an Exclusion Test of Low Torsion Bound Densities

The heaviest well-measured neutron stars, at about two solar masses, are the densest stable matter configurations known, and their existence is a standing experiment on any theory that modifies matter at high density. In a torsion-regulated framework, the spin-torsion term softens and eventually reverses the effective gravity of compressed matter at a bound density; if that bound density lay within the range neutron stars actually reach, their structure and maximum mass would be altered beyond what observations allow. This paper converts the two-solar-mass fact into an exclusion. With central densities up to 2e+18 kg per cubic metre in the heaviest stars, any operative torsion bound density below 2e+18 kg per cubic metre is excluded. On the neutron branch of the Aldred bound, at 9.72e+57 kg per cubic metre, the fractional torsion correction at a central density of 1e+18 kg per cubic metre is 1.03e-40 — the stars are entirely unaffected, as their ordinary appearance requires. Expressed as a carrier-mass statement, the exclusion requires any confined fermion that sets an operative bound to be heavier than 1.35e-11 eV per c squared at full polarisation, weakening to 1.35e-10 eV per c squared if the polarised fraction is only 0.1 — numbers so small that the paper states plainly the mass form of the bound is nearly empty, while its density form is a real and usable fence against modified torsion models. Computed from stated assumptions, not measured.