Abstract
Soon after the discovery by Hawking in 1974 that a black hole formed by gravitational collapse will radiate a thermal distribution of field quanta, a number of authors showed that, in particular spacetimes, when a quantum field is in a certain “natural vacuum state,” then appropriate observers “see” a thermal distribution of particles. For the ordinary vacuum state of Minkowski spacetime, Unruh (1976) obtained such a result for accelerating observers. In extended Schwarzschild spacetime, Hartle and Hawking (1976) and Israel (1976) defined a natural vacuum state (the “Hartle-Hawking vacuum”), which is a thermal state for a static observer. Similarly, for de Sitter spacetime, Gibbons and Hawking (1977) defined the “Euclidean vacuum state” and showed that it has thermal properties for any inertial (geodesic) observer.
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Wald, R.M. (1990). Vacuum States in Spacetimes with Killing Horizons. In: Audretsch, J., de Sabbata, V. (eds) Quantum Mechanics in Curved Space-Time. NATO ASI Series, vol 230. Springer, Boston, MA. https://doi.org/10.1007/978-1-4615-3814-1_8
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DOI: https://doi.org/10.1007/978-1-4615-3814-1_8
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