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IndisputableMonolith.Gravity.BlackHoleInformationPreservation

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This module defines the black-hole mass at time t under linear evaporation in RS-native units, together with evaporation time, entropy sums, and radiation entropy. Researchers working on the black-hole information paradox within Recognition Science would cite these quantities. The module is a collection of definitions and short lemmas with no complex proofs.

claimThe black-hole mass at time $t$ under linear evaporation is $M(t) = M_0 (1 - t/t_{ m evap})$ for $0 \le t \le t_{ m evap}$, with $t_{ m evap}$ the evaporation timescale, $S_{ m BH}(t)$ the horizon entropy from the ledger, and $S_{ m rad}(t)$ the radiated entropy.

background

The module imports the RS time quantum $ au_0 = 1$ tick from Constants. It relies on the ledger-derived Bekenstein-Hawking entropy $S_{ m BH} = A/(4 au_0^2)$ with $\phi$-rational log corrections from BlackHoleEntropyFromLedger, the Hawking temperature expressed via rung spacing from HawkingTemperatureFromRung, and the bounce-echo identity from BlackHoleEchoesFromBounce. The local setting is the discrete RS ledger applied to Schwarzschild horizons under the linear-evaporation ansatz.

proof idea

This is a definition module, no proofs.

why it matters in Recognition Science

The definitions supply the mass evolution and entropy accounting required for the black-hole information-preservation argument in the Recognition Science framework. They connect the entropy-from-ledger result and the temperature-from-rung result to the overall information accounting that closes the paradox via the bounce-echo mechanism.

scope and limits

depends on (5)

Lean names referenced from this declaration's body.

declarations in this module (31)