Spin-Sourced Torsion in Pulsars and Magnetars: A Null Result With Its Margin Printed

In Einstein-Cartan gravity, torsion is sourced by the intrinsic spin density of matter. This paper computes, in the frame defined by the Aldred Limit (rho_A = 9.72e54 g/cm^3), the spin-density and pulsar-timing consequences for a canonical pulsar, a millisecond pulsar, and a magnetar, under both full (unphysical, upper-bound) and realistic Pauli-paramagnetic polarisation of the neutron-star core. The result is negative and is printed at full size: the quadratic spin-torsion fractional correction is 2.06e-40 at full alignment and 1.03e-40 at realistic polarisation (forty orders of magnitude below unity); accumulated spin-down timing residuals over ten years fall short of the best achieved precision (100 ns, nanosecond class) by about 32 orders of magnitude; and even a deliberately generous linear precession envelope remains 2.4-4.7 orders of magnitude below achieved precision at full alignment and 8.7-14.1 orders below it at realistic polarisation. Detection would require a central density of order 1e47 g/cm^3. The spin-torsion timing channel in neutron stars is closed. All computations are reproducible from the deposited script (compute.py, results.txt, results.json). Drafted with the assistance of Dave, an AI research system; all computations reproducible from the included script.