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A black hole’s gravity prevents escape of anything, including light, once the event horizon forms.
A black hole is an extremely compact astronomical object whose gravity is so strong that nothing can escape, not even light. In general relativity, this happens when a sufficiently compact mass collapses so that a boundary called the event horizon forms; once an object crosses it, it becomes trapped inside and cannot send information back to the outside universe. The event horizon is therefore the “no escape” surface, and its existence is central to how black holes are defined and understood. General relativity also predicts that black holes contain a central singularity where spacetime curvature becomes infinite (ignoring quantum effects). Historically, the idea that light could be unable to escape from a massive body was considered in the late 18th century by Michell and Laplace, but the modern framework came from Einstein’s theory of general relativity and the Schwarzschild solution. Physically, black holes are studied through their effects on surrounding matter and radiation—such as accretion disks, gravitational lensing, and gravitational waves from mergers—since the interior cannot be observed directly.
A black hole’s gravity prevents escape of anything, including light, once the event horizon forms.
The event horizon is the defining boundary: crossing it traps objects inside with no locally detectable change at the horizon.
General relativity predicts a central singularity with infinite spacetime curvature (when quantum effects are ignored).
Black holes are identified indirectly via their interactions with matter and electromagnetic radiation, and by gravitational waves from mergers.
The boundary of a black hole beyond which matter and light can pass only inward, so nothing can escape to the outside.
A region inside a black hole where spacetime curvature becomes infinite in classical general relativity (ignoring quantum effects).
The characteristic radius of a non-rotating black hole at which the event horizon forms, given by r_s = 2GM/c^2.
The bending of light caused by a massive object’s gravity, used to infer the presence of compact objects like black holes.
Quantum-predicted radiation emitted by black holes from the event horizon, with a rate inversely related to the black hole’s mass.
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