Hawking Radiation & Black Hole Evaporation

Stephen Hawking (1974): black holes emit thermal radiation at temperature T_H = ℏc³/(8πGMk_B). Virtual particle pairs at the horizon — one falls in, one escapes. The black hole slowly evaporates, shrinking as it radiates.

Initial Mass M₀80 M☉

Simulation Speed

Hawking Temperature: T_H = ℏc³/(8πGMk_B) ∝ 1/M
Evaporation time: t_evap = 5120πG²M³/(ℏc⁴) ∝ M³
Entropy: S = A/4l_P² = 4πGM²/(ℏc) — Bekenstein-Hawking
A solar-mass BH has T_H ≈ 60 nK — far colder than CMB (2.7 K)