The Chandrasekhar Mass Corrected by the Electron-Branch Density Bound

The Chandrasekhar mass is the best-known density-related bound in stellar astrophysics, so it is the natural first place to ask whether a spin-torsion density ceiling changes a stellar limit. This paper recomputes the limiting mass of 1.456 solar masses for a mean molecular weight per electron of two, places finite central densities for near-limit white dwarfs between 1e9 and 1e13 kg per cubic metre against the electron-branch bound of 2.87e+48 g per cubic centimetre, and bounds the resulting shift. At a representative central density of 1e12 kg per cubic metre the fractional correction is 3.48e-40, so the limiting mass moves by at most 5.07e-40 solar masses; even at 1e13 kg per cubic metre the fraction is only 3.48e-39. Composition changes matter far more: an iron composition lowers the standard limit to 1.255 solar masses. The density bound therefore leaves the Chandrasekhar mass unchanged at every quoted precision. Computed from stated assumptions, not measured.