A Temperature Ceiling for Evaporating Black Holes Set by the Density Cap

The ceiling is 1.417e+12 kelvin at the remnant mass of 8.659e+10 kilograms. For orientation, a ten-solar-mass hole radiates at 6.170e-09 kelvin and a solar-mass hole at 6.170e-08 kelvin, while a hole of 1e12 kilograms reaches 1.227e+11 kelvin. The ceiling converts, through Boltzmann's constant, to a characteristic particle energy of about a tenth of a giga-electronvolt rather than anything near the Planck scale, which places the final evaporation stage in a regime where known particle physics, not speculative physics, governs the emitted species. That placement matters for observation. Computed from stated assumptions, not measured.