Central Densities Along the White Dwarf Sequence Compared with the Electron-Branch Bound

White dwarfs span a wide range of central densities along their mass sequence, and the most massive of them are the densest stable stars short of neutron stars. This paper computes radii from the standard mass-radius relation, estimates central densities with a polytropic concentration factor, and places six masses from 0.4 to 1.35 solar masses against the electron-branch density bound. A one-solar-mass dwarf has a radius of 5.643e+03 km and a central density of 7.17e+10 kg per cubic metre, a fraction 2.49e-41 of the bound. The most massive model, at 1.35 solar masses, reaches a central density of 1.85e+12 kg per cubic metre and a fraction of 6.42e-40. The whole white dwarf sequence, end to end, occupies the lowest approach to its operative bound of any stellar family. Simulated from stated assumptions, not measured.