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The fate of Schwarzschild-de Sitter Black Holes in f(R) gravity
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The fate of Schwarzschild-de Sitter Black Holes in f(R) gravity
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The semiclassical effects of antievaporating black holes can be discussed in the framework of $f(R)$ gravity. In particular, the Bousso-Hawking-Nojiri-Odinstov antievaporation instability of degenerate Schwarzschild-de Sitter black holes (the so called Nariai space-time) leads to a dynamical increasing of black hole horizon in $f(R)$ gravity. This phenomenon causes the following transition: emitting marginally trapped surfaces become space-like surfaces before the effective Bekenstein-Hawking emission time. As a consequence, Bousso-Hawking thermal radiation cannot be emitted in an antievaporating Nariai black hole. Possible implications in cosmology and black hole physics are also discussed.
Forward citations
Cited by 2 Pith papers
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The Fate of Nucleated Black Holes in de Sitter Quantum Gravity
Nucleated maximal-mass black holes in de Sitter space undergo thermal Hawking evaporation in smooth quantum states and return fully to the empty de Sitter vacuum.
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The Fate of Nucleated Black Holes in de Sitter Quantum Gravity
Nucleated black holes in de Sitter space evaporate via standard Hawking radiation back to the empty vacuum, rendering nucleation a temporary fluctuation.
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