Temperature: T = ℏc³ / (8πGMkB). Ideal lifetime: τ = 5120πG²M³ / (ℏc⁴). At fixed assumptions, T ∝ 1/M, power ∝ 1/M² and remaining lifetime ∝ M³.
The lifetime coefficient uses an ideal horizon-area blackbody approximation. Real calculations include frequency-dependent transmission (greybody factors) and available particle species; spin, charge and the environment also change the history. Treat the table as an order-of-magnitude teaching estimate.
The evaporation segment solves M³ = M₀³(1 − t/τ). It zooms logarithmically from 100% to 1% of the initial mass; it does not simulate the final quantum-gravity stage. The separate final chapter is a question, not a computed disappearance.
The live WebGL view numerically bends light around a non-spinning black hole in Schwarzschild geometry. The turbulent disk texture, brightness and bloom are artistic; this is not a fluid simulation or an observed image. Disk fading, star fading and camera size illustrate the story. In the dark eras a faint contour locates the hole; the blue radiation glow is greatly exaggerated and is not the visible colour or brightness of Hawking radiation. The non-WebGL fallback is a simpler 2D illustration. Hawking radiation from astrophysical black holes has not been directly detected. No flashes or particle-pair cartoon are presented as a measured mechanism.
“The last” is a scenario, not an identified object. Far-future claims assume a broadly continuing, cooling Universe; the fate of dark energy, proton decay, future mergers and quantum gravity is not settled.