Black Holes Explained – From Birth to Death

Supernova explosions create the universe's heavy elements because the implosion and explosive reheating generate the extreme temperatures, densities, and neutron fluxes needed to fuse nuclei beyond iron and disperse them into space.

Supermassive black holes will outlive any observers because Hawking evaporation scales so steeply with mass that the largest black holes require vastly more than the universe's current age—often by many orders of magnitude—to evaporate.

Hawking evaporation accelerates as a black hole shrinks because its temperature rises inversely with mass, so smaller black holes radiate more power and lose mass faster, culminating in a rapid final phase.

Black holes evaporate via Hawking radiation because quantum vacuum fluctuations near the horizon can separate particle–antiparticle pairs so one escapes as real radiation while the other falls in, and that escaping radiation carries away energy and mass.

How quickly you die approaching a black hole depends on its mass because tidal gradients at the horizon scale inversely with size, so small black holes can destroy you at or before the horizon while supermassive ones have much gentler horizons.

The firewall hypothesis would destroy infalling matter almost at the horizon because proposed quantum effects create a region of extremely high-energy quanta there that would interact violently and vaporize anything crossing.

Tidal forces near a black hole tear objects apart because gravitational acceleration changes dramatically over tiny distances, stretching and eventually shredding matter into plasma.

Inside the event horizon you are forced toward the singularity because the curvature of spacetime makes the inward radial direction timelike, so all future-directed paths lead closer to the center regardless of any propulsion.