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Hawking radiation is black body radiation that is theorized to be released outside a black hole's event horizon because of relativistic quantum effects. It is named after the physicist Stephen Hawking, who developed a theoretical argument for its existence in 1974. Hawking radiation is a purely kinematic effect that is generic to Lorentzian geometries containing event horizons or local apparent horizons. Hawking radiation reduces the mass and rotational energy of black holes and is therefore also theorized to cause black hole evaporation. Because of this, black holes that do not gain mass through other means are expected to shrink and ultimately vanish. For all except the smallest black holes, this would happen extremely slowly. The radiation temperature is inversely proportional to the black hole's mass, so micro black holes are predicted to be larger emitters of radiation than larger black holes and should dissipate faster.
Hawking's discovery followed a visit to Moscow in 1973, where the Soviet scientists Yakov Zel'dovich and Alexei Starobinsky convinced him that rotating black holes ought to create and emit particles, while Russian physicist Vladimir Gribov believed that even a non-rotating black hole should emit radiation. When Hawking did the calculation, he found to his surprise that it was true. In 1972, Jacob Bekenstein conjectured that the black holes should have an entropy,[9] where by the same year, he proposed no-hair theorems. Bekenstein's discovery and results are commended by Stephen Hawking, which also led him to think about radiation due to this formalism.
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