Αποτελέσματα Αναζήτησης
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 of a black hole: S bh = S BH ≡ 1 4 A. (2) Here the subscript bh stands for “black hole,” and the subscript BH stands for “Bekenstein-Hawking.”
The Hawking temperature of a black hole is such that the Wien wave length corresponds to the radius of the black hole itself. We assume basic knowledge of Special Relativity, assuming c = 1 for our unit system
C. The spectrum of Hawking radiation We want to equate hA "( )A "( 0)i vac:subtr: to an integral of the type Eq. (16) without the +1 2 contribution due to vacuum uctuations (which we have already subtracted). It is easiest to do this if we use the identity: sinhx x = Y1 n=1 1 + x2 (ˇn)2 ; (22)
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
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
25 Μαΐ 2022 · in all directions a type of thermal radiation known as Hawking radiation. According to Hawking’s calculations, for an observer located at a large distance from the horizon (ideally infinite), this radiation has a blackbody spectrum whose abso-lute temperature is Hawking temperature: T H = ˜c3 8πkGM BH (2) where ˜ = h/2π = 1.05×10−34 J ...
Stephen Hawking (b.1942) studied the quantum theory of electromagnetism near black holes, he found that black holes actually emit radiation, that in fact has a black-body spectrum. How can black holes emit radiation? It should be no surprize that the answer lies in quantum uncertainty. All over spacetime the quantum electromagnetic eld
