Hawking radiation is the thermal radiation predicted to be spontaneously emitted by black holes. It arises from the steady conversion of quantum vacuum fluctuations into pairs of particles, one of which escaping at infinity while the other is trapped inside the black hole horizon. It is named after the physicist Stephen Hawking who derived its existence in 1974. This radiation reduces the mass of black holes and is therefore also known as black hole evaporation.
Contents
1 Black hole formation
2 Black hole horizon properties
3 Redshift and structure of outgoing light rays
4 Quantum mechanics and Hawking radiation
5 The origin of Hawking radiation
6 Observing Hawking radiation
7 Quantum gravity and the role of very short distance effects
8 Footnotes
9 References
10 See Also
Black hole formation
There are two kinds of black holes in the Universe: those of stellar origin of a few solar masses, and those found in globular clusters or in galactic nuclei. The second are much more massive; their masses vary between a few hundred and a billion solar masses. The first type are better known, and we briefly review how they form. When a sufficiently massive star has burned its nuclear material, its internal pressure is no longer able to resist its own gravitational attraction. As a result, the star implodes. The outer layers bounce off the inner ones and a large fraction of the star's matter is ejected at a speed on the order of a few percent of the speed of light c . The star undergoes a supernova. It will then contract and, if the residual material is not too massive, a new equilibrium state will be reached: a neutron star. But if the mass is greater than a few solar masses, the pressure will not be able to counterbalance its weight. It will thus ineluctably keep collapsing and form a black hole.
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Hawking radiation is black body radiation emitted by a black hole, caused by quantum effects near the event horizon.
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