![]() ![]() Several theories were subsequently developed, some with and some without event horizons. ![]() In 1958, David Finkelstein used general relativity to introduce a stricter definition of a local black hole event horizon as a boundary beyond which events of any kind cannot affect an outside observer, leading to information and firewall paradoxes, encouraging the re-examination of the concept of local event horizons and the notion of black holes. In these theories, if the escape velocity of the gravitational influence of a massive object exceeds the speed of light, then light originating inside or from it can escape temporarily but will return. At that time, the Newtonian theory of gravitation and the so-called corpuscular theory of light were dominant. In 1784, John Michell proposed that gravity can be strong enough in the vicinity of massive compact objects that even light cannot escape. Wolfgang Rindler coined the term in the 1950s. In astrophysics, an event horizon is a boundary beyond which events cannot affect an observer. ![]()
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