发表机构
Columbia University; University of Michigan; University of California, Los Angeles; University of Pennsylvania（哥伦比亚大学; 密歇根大学; 加州大学洛杉矶分校; 宾夕法尼亚大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文研究霍金振幅计算中半经典与弱场近似的可交换性问题，解决鞍点分析的微妙之处，实现多黑洞背景下半经典霍金振幅计算，并提出基于斯托克斯线确定热谱温度的新方法。
AI 中文摘要
霍金振幅提供了一种利用散射振幅文献中的壳上技术确定黑洞霍金谱的新方法。本文研究了此前用于计算霍金振幅的半经典近似与弱场近似之间的相互作用，发现这些极限未必可交换，凸显了支配半经典极限的鞍点分析存在的微妙之处。解决这些问题使我们能够在包括Tangherlini度规、Reissner-Nordström度规和Hernquist度规在内的一系列黑洞背景中计算半经典霍金振幅。此外，我们描述了不同能量下主导霍金振幅的鞍点贡献，并提出了一种基于霍金振幅的斯托克斯线确定所得热谱温度的新方法。
英文摘要
Hawking amplitudes provide a new way of determining the Hawking spectrum of black holes, using on-shell techniques borrowed from the literature on scattering amplitudes. In this paper, we investigate the interplay between the semi-classical and weak-field approximations previously used to compute Hawking amplitudes. We find that these limits do not necessarily commute, highlighting subtleties with the saddle point analyses governing the semi-classical limit. Resolving these issues allows us to compute semi-classical Hawking amplitudes in a range of black-hole backgrounds, including Tangherlini, Reissner-Nordström, and Hernquist metrics. Moreover, we describe the saddle-point contributions dominating Hawking amplitudes for different energies and propose a new method for determining the temperature of the resulting thermal spectrum based on Stokes lines of Hawking amplitudes.
Comments39 pages, 5 figures
