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arXiv 1409.0144hep-thgr-qc
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引力坍缩中的纠缠熵产生:协变正则化和可解模型

Entanglement entropy production in gravitational collapse: covariant regularization and solvable models

Eugenio Bianchi, Tommaso De Lorenzo, Matteo Smerlak

摘要:

研究了引力坍缩及随后的黑洞蒸发过程中真空纠缠的动力学性质。在论文的第一部分中,我们引入了一种适用于弯曲时空的纠缠熵的协变正则化,这种正则化使我们能够对黑洞的“外部熵”和“辐射熵”的概念给出精确的定义。“对于Vaidya坍缩模型,我们发现结果与霍金辐射的标准热力学性质一致。在论文的第二部分中,我们计算了各种球对称时空的真空纠缠熵,包括Barnesi,Hayward,Frolov和Rovelli-Vidotto的非奇异黑洞模型和Haggard-Rovelli的“黑洞烟花”模型。我们具体讨论的作用,事件和捕获视界与行为的辐射熵在未来的零无穷大。我们特别观察到,$(i)$在事件视界的存在下,辐射熵在蒸发过程结束时发散,$(ii)$在非奇异蒸发模型中(具有捕获区域但没有事件视界)广义第二定律仅在早期成立并且在“净化”阶段被违反,在后期,辐射熵可以变为负值,(即,辐射可以比真空更少相关),然后回到零,导致上下-研究了酉蒸发黑洞的Page曲线的向上行为。

英文摘要:

We study the dynamics of vacuum entanglement in the process of gravitational collapse and subsequent black hole evaporation. In the first part of the paper, we introduce a covariant regularization of entanglement entropy tailored to curved spacetimes; this regularization allows us to propose precise definitions for the concepts of black hole "exterior entropy" and "radiation entropy." For a Vaidya model of collapse we find results consistent with the standard thermodynamic properties of Hawking radiation. In the second part of the paper, we compute the vacuum entanglement entropy of various spherically-symmetric spacetimes of interest, including the nonsingular black hole model of Bardeen, Hayward, Frolov and Rovelli-Vidotto and the "black hole fireworks" model of Haggard-Rovelli. We discuss specifically the role of event and trapping horizons in connection with the behavior of the radiation entropy at future null infinity. We observe in particular that $(i)$ in the presence of an event horizon the radiation entropy diverges at the end of the evaporation process, $(ii)$ in models of nonsingular evaporation (with a trapped region but no event horizon) the generalized second law holds only at early times and is violated in the "purifying" phase, $(iii)$ at late times the radiation entropy can become negative (i.e. the radiation can be less correlated than the vacuum) before going back to zero leading to an up-down-up behavior for the Page curve of a unitarily evaporating black hole.

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