Hawking radiation. Hawking radiation is black body radiation that is predicted to be released by black holes, due to quantum effects near the event horizon.
It is named after the physicist Stephen Hawking, who provided a theoretical argument for its existence in 1974,[1] and sometimes also after Jacob Bekenstein, who predicted that black holes should have a finite, non-zero temperature and entropy.[2] Hawking's work followed his visit to Moscow in 1973 where the Soviet scientists Yakov Zeldovich and Alexei Starobinsky showed him that according to the quantum mechanical uncertainty principle, rotating black holes should create and emit particles.[3] Hawking radiation reduces the mass and the energy of the black hole and is therefore also known as black hole evaporation.
Because of this, black holes that lose more mass than they gain through other means are expected to shrink and ultimately vanish. Overview[edit] The LHC, Black Holes and You : Starts With A Bang. Who is correct here?
We don’t know, you don’t know, it is uncharted territory. Would you bet the entire human history and the existence of our solar system on it? I wouldn’t. –from a user comment on my old website on the topic of the Large Hadron Collider. LHCMilestones-en. Black hole. A black hole is defined as a region of spacetime from which gravity prevents anything, including light, from escaping.[1] The theory of general relativity predicts that a sufficiently compact mass will deform spacetime to form a black hole.[2] Around a black hole, there is a mathematically defined surface called an event horizon that marks the point of no return.
The hole is called "black" because it absorbs all the light that hits the horizon, reflecting nothing, just like a perfect black body in thermodynamics.[3][4] Quantum field theory in curved spacetime predicts that event horizons emit radiation like a black body with a finite temperature. This temperature is inversely proportional to the mass of the black hole, making it difficult to observe this radiation for black holes of stellar mass or greater. Objects whose gravity fields are too strong for light to escape were first considered in the 18th century by John Michell and Pierre-Simon Laplace.