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 in charged linear dilaton black holes
2 Pith papers cite this work. Polarity classification is still indexing.
abstract
We investigate the Page curve for a non-standard black hole which is asymptotically non-flat/AdS/dS. For this purpose, we apply the island prescription to the charged linear dilaton black holes and analyze, in detail, the entanglement entropy of Hawking radiation for both the non-extremal case and the extremal case. In the non-extremal case, we find the Page curve consistent with the unitarity principle: at early times the entanglement entropy grows linearly in time without the island and at late times it is saturated double of the Bekenstein-Hawking entropy in the presence of the island. We observe the Page time is universal for all different models studied by our method: $t_{\text{Page}}=\frac{3}{ \pi c}\frac{S_{\text{BH}}}{T_H}.$ For the extremal case, the island prescription provides the well defined entanglement entropy only with the island, which can not be obtained from the continuous limit of the non-extremal case. This implies that the Page curve may not be reproduced for the extremal case and further investigation is needed.
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hep-th 2years
2026 2roles
background 1polarities
background 1representative citing papers
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.