根據島規則，糾纏熵在半古典重力可以分為來自量子效應與重力的貢獻。 其中量子效應可以用Ryu–Takayanagi公式來得到，而重力部分等於量子極面(quantum extremal surface)除以四倍的牛頓常數。 我們展示了在此全像系統演化晚期，糾纏熵成長是線性的。 過了佩吉時間(Page time)，量子極面出現並且系統達到飽和。在這篇論文中，我們將強調在任意維度的時空，黑洞旋轉如何如何引響其糾纏熵。;We study the time evolution of the entanglement entropy of Hawking radiation in the (n+1)-dimensional Kerr-Newman black hole evaporation by the holographic approach that considering the (n+1)-dimensional AdS eternal black brane coupled to the auxiliary CFT reservoir is in the Hartle-Hawking state. The CFT reservoir itself has a holographic dual, the (n+2)-dimensional bulk geometry, and the original (n+1)-dimensional AdS-black brane is embedded into such bulk manifold, which is precisely Randall–Sundrum model.
According to the island rule, the entanglement entropy in semi-classical gravity can be divided into two parts, one is due to the quantum effects, which can be obtained by Ryu–Takayanagi conjecture. Another is the gravitational part, which is equal to the area of the quantum extremal surface divided by four times the Newton′s constant. We show that the entanglement growth in our holographic system is linear in late times. After Page time, the system reaches saturation since the entanglement islands appear. In this thesis, we will emphasize how black hole rotation affects entanglement entropy in general dimensional spacetime.
