Black-Hole Bookkeeping in the Aldred Frame: The Bounced Core, the Remnant Floor, and What Evaporation Leaves Behind

Mass and entropy bookkeeping for black holes in Einstein-Cartan spin-torsion gravity with the Aldred Limit rho_A = 9.72e54 g/cm^3. (a) A mass M accumulated at rho_A occupies R_A(M) = [3M/(4 pi rho_A)]^(1/3) (3.66e-8 cm at one solar mass); at first touch, under a stated uniform-core plus power-law-envelope profile with index alpha = 2, the bounced core has radius 7.42e-15 cm and mass 1.67e13 g independent of progenitor mass, while across alpha in [1.5, 2.5] the first-touch mass fraction spans some 32 orders of magnitude and is therefore a property of the profile, not of the frame. (b) Hawking evaporation has a floor: the horizon encloses mean density rho_A at M_rem = [3 c^6/(32 pi G^3 rho_A)]^(1/2) = 8.66e13 g = 3.98e18 Planck masses (horizon radius 1.29e-14 cm, Hawking temperature 1.42e12 K); centrally concentrated cores raise the floor as f^(-1/2), to 6.37e14 g for an n = 3 polytropic concentration. (c) At the remnant mass the frame and the standard singular picture assign the same Bekenstein-Hawking entropy, S/k_B = 1.99e38, which is 3.85 times the remnant's baryon-count entropy scale; the retained capacity is a fraction (M_rem/M)^2 = 1.90e-41 of a ten-solar-mass hole's initial entropy, so the bookkeeping relocates the evaporation endpoint without claiming to resolve the information question. All numbers are produced by the deposited compute.py. AI-use disclosure: this paper was prepared with the assistance of Dave, an AI system built by Aldred Industries; all computations were performed and checked by script, and the author of record reviewed the results.