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Hawking found that the black hole temperature was T = κ/(2π), so ǫ = 1/(2π) and hence η = 1/4. This gives the famous Bekenstein-Hawking formula for the entropy
25 Μαΐ 2022 · In 1974, Stephen Hawking theoretically discovered that black holes emit thermal radiation and have a characteristic temperature, known as the Hawking temperature. The aim of this paper is to present a simple heuristic derivation of the Hawking temperature, based on the Heisenberg uncertainty principle.
Hawking has theorized that during pair produc-tion occurring just outside the event horizon, a black hole slowly loses mass or evaporates as particles are radiated away. This, now known as “Hawking radia-tion,” was initially described to many in his first popular book A Brief History of Time. In this
so-called \Hawking radiation" would be a property that all black holes have in common, though for the astronomical black holes it would be far too weak to be observed directly. The radiation is purely thermal. The Hawking temperature of a black hole is such that the Wien wave length corresponds to the radius of the black hole itself.
but is intended to be the simplest way to get Hawking radiation. The key point is that all outgoing waves in the system arose from ingoing waves that just barely managed to make it back out before they crossed the horizon; the
Hawking radiation is the theoretical emission released outside a black hole's event horizon. This is counterintuitive because once ordinary electromagnetic radiation is inside the event horizon, it cannot escape. It is named after the physicist Stephen Hawking, who developed a theoretical argument for its existence in 1974. [1]
black hole radiation. In 1974, Stephen Hawking showed that black holes, which are objects that light cannot escape from and hence classically are at absolute zero, do radiate at temperature T H= ~c3 8ˇGMk b; (1.0.1) when quantum mechanical e ects are taken into account. The presence of both gravitational and quantum mechanical constants re
