Fuzzball models with stretched horizons modify or eliminate entanglement islands depending on boundary conditions and cap geometry, producing information paradox analogues in some cases.
Islands and Page curves of Reissner-Nordstr\"om black holes
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abstract
We apply the recently proposed quantum extremal surface construction to calculate the Page curve of the eternal Reissner-Nordstr\"om black holes in four dimensions ignoring the backreaction and the greybody factor. Without the island, the entropy of Hawking radiation grows linearly with time, which results in the information paradox for the eternal black holes. By extremizing the generalized entropy that allows the contributions from the island, we find that the island extends to the outside the horizon of the Reissner-Nordstr\"om black hole. When taking the effect of the islands into account, it is shown that the entanglement entropy of Hawking radiation at late times for a given region far from the black hole horizon reproduces the Bekenstein-Hawking entropy of the Reissner-Nordstr\"om black hole with an additional term representing the effect of the matter fields. The result is consistent with the finiteness of the entanglement entropy for the radiation from an eternal black hole. This facilitates to address the black hole information paradox issue in the current case under the above-mentioned approximations.
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hep-th 2years
2026 2roles
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A rotating regular black hole leaves a remnant because the correction term in the generalized entropy of Hawking radiation vanishes at a finite mass above the extremal limit.
citing papers explorer
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Entanglement islands, fuzzballs and stretched horizons
Fuzzball models with stretched horizons modify or eliminate entanglement islands depending on boundary conditions and cap geometry, producing information paradox analogues in some cases.
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The Remnant of an Evaporating Rotating Regular Black Hole from the Generalized Entropy in the Final Stage of Evaporation
A rotating regular black hole leaves a remnant because the correction term in the generalized entropy of Hawking radiation vanishes at a finite mass above the extremal limit.