Pure de Sitter space and the island moving back in time
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Publication:5162822
DOI10.1088/1361-6382/ABFF9AzbMATH Open1482.83109arXiv2008.07994OpenAlexW3161638994MaRDI QIDQ5162822
Author name not available (Why is that?)
Publication date: 5 November 2021
Published in: (Search for Journal in Brave)
Abstract: Observers in de Sitter space can only access the space up to their cosmological horizon. Assuming thermal equilibrium, we use the quantum Ryu-Takayanagi or island formula to compute the entanglement entropy between the states inside the cosmological horizon and states outside, as a function of time. We obtain a Page curve that is bound at a value corresponding to the Gibbons-Hawking entropy. At this transition an 'island' forms, which is in a significantly different location as compared to when considering black hole horizons and even moves back in time. These differences turn out to be essential for non-violation of the no-cloning theorem in combination with entanglement wedge reconstruction. This consideration furthermore introduces the need for a scrambling time, the entropy dependence of which turns out to coincide with what is expected for black holes. The model we employ has pure three-dimensional de Sitter space as a solution. We dimensionally reduce to two dimensions in order to take into account semi-classical effects. Nevertheless, we expect the aforementioned qualitative features of the island to persist in higher dimensions.
Full work available at URL: https://arxiv.org/abs/2008.07994
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