What is the Bekenstein-Hawking entropy formula, and how does it relate to the black hole's surface area and event horizon?

What Boltzmann's entropy formula states — S = k ln Ω, connecting microscopic states to macroscopic entropy

Boltzmann's formula relates entropy (S) to the natural logarithm of the number of microstates (Ω), with k as Boltzmann's constant

What Hawking radiation implies — black holes have a temperature and slowly evaporate over time

Hawking radiation suggests black holes emit thermal radiation, gradually diminishing

What the information paradox asks — does information falling into a black hole disappear, violating quantum mechanics

The information paradox questions: Does information vanish in black holes, contradicting quantum theory?

What the Kerr solution adds — spacetime around a rotating black hole, including frame-dragging

Kerr solution describes rotating black holes' spacetime, featuring frame-dragging effects

What the Einstein field equations relate — the curvature of spacetime (Gμν) to the energy-momentum tensor (Tμν)

Einstein's field equations: Gμν = 8πTμν, relating spacetime curvature to energy-momentum

What the second law of thermodynamics says — entropy of an isolated system never decreases

Entropy in an isolated system always increases or remains constant