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arXiv 1408.6005hep-th
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时空纠缠的全息方法

A Holographic Approach to Spacetime Entanglement

Jason Wien

摘要:

最近有人提出,时空视界熵的贝肯斯坦-霍金公式在作为基础的量子理论中,作为对一般时空区域的纠缠熵的主要贡献,具有更大的意义[2]。这个"时空纠缠猜想"有一个全息实现,它将任意类空余维2表面上的熵公式与边界上特定余维2区域族的微分熵等同起来。微分熵可以被认为是纠缠熵沿一族表面的方向导数。这种全息关系首先在[3]中进行了研究,并在[4]中进行了扩展,并且在[4]中证明了它在爱因斯坦引力中对于具有平面对称性的体表面(以及某些更高曲率的理论)是成立的。在这篇文章中,我们回顾了这一证明,并提供了明确的例子,如何建立一个给定的体积曲线的适当的家庭的边界区间。相反,给定一个家庭的边界区间,我们提供了一种方法来构建相应的体积曲线的纠缠楔边界的交叉点。我们的工作主要是在三个方面,并评论如何建设扩展到更高的维度。

英文摘要:

Recently it has been proposed that the Bekenstein-Hawking formula for the entropy of spacetime horizons has a larger significance as the leading contribution to the entanglement entropy of general spacetime regions, in the underlying quantum theory [2]. This `spacetime entanglement conjecture' has a holographic realization that equates the entropy formula evaluated on an arbitrary space-like co-dimension two surface with the differential entropy of a particular family of co-dimension two regions on the boundary. The differential entropy can be thought of as a directional derivative of entanglement entropy along a family of surfaces. This holographic relation was first studied in [3] and extended in [4], and it has been proven to hold in Einstein gravity for bulk surfaces with planar symmetry (as well as for certain higher curvature theories) in [4]. In this essay, we review this proof and provide explicit examples of how to build the appropriate family of boundary intervals for a given bulk curve. Conversely, given a family of boundary intervals, we provide a method for constructing the corresponding bulk curve in terms of intersections of entanglement wedge boundaries. We work mainly in three dimensions, and comment on how the constructions extend to higher dimensions.

机构、总结、中文摘要均由AI分析而来,可能存在错误,请以论文正文为准。

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