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This boundary marks the point of no return around a black hole, beyond which nothing—not even light—can escape.
This famous physicist's equations from 1915 first predicted the existence of black holes as a consequence of curved spacetime.
This is the term for the swirling disk of gas and matter that spirals around a black hole before falling in.
This type of black hole forms when a massive star collapses at the end of its life in a supernova explosion.
This is the infinitely dense point at the very center of a black hole where all the mass is concentrated.
This is the common term for the enormous black holes found at the centers of most galaxies, with masses millions to billions times that of the Sun.
This British physicist theorized that black holes emit radiation and slowly evaporate over time, a process now named after him.
This force, one of the four fundamental forces of nature, is responsible for creating and shaping black holes.