发表机构
Lanzhou University; Shaoxing Institute of Technology（兰州大学; 绍兴文理学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文采用Kerr/CFT方法分析正则极值黑洞弹跳时空（Kerr、Kerr-Newman、Reissner-Nordström对应物）的中心荷与黑洞熵，发现Cardy公式计算的微观熵与贝肯斯坦-霍金熵一致，验证了该方法在无奇点正则时空中的有效性。
AI 中文摘要
贝肯斯坦-霍金熵正比于视界面积的四分之一，是黑洞热力学的基础，也可通过AdS/CFT对应来理解，例如三维BTZ黑洞与二维CFT。在本工作中，我们采用Kerr/CFT方法分析正则极值黑洞弹跳时空（包括Kerr、Kerr-Newman和Reissner-Nordström黑洞的对应物）的中心荷与黑洞熵。这些时空在$r=0$处无曲率奇点。我们推导了这些时空的近视界几何，发现它们具有增强的对称性，即SL$(2,\mathbb{R})\times \mathrm{U}(1)$或SL$(2,\mathbb{R}) \times \mathrm{SO}(3)$。通过施加适当的边界条件，我们分析了它们的渐近对称群，其中包含微分同胚以及由电磁场产生的$\mathrm{U}(1)_{\rm gauge}$对称性。然后我们从荷代数中提取中心荷，并评估Frolov-Thorne真空的左移温度。值得强调的是，在黑洞弹跳Kerr-Newman情形中，来自电磁贡献的中心荷为零。此外，在黑洞弹跳Reissner-Nordström情形中，我们通过加入一个$\mathrm{U}(1)$规范纤维将4D几何提升为5D构型。我们的结果表明，由Cardy公式计算的微观熵与贝肯斯坦-霍金熵一致。这一一致性表明Kerr/CFT方法对某些无曲率奇点的正则时空仍然有效，从而为黑洞熵提供了微观统计理解。
英文摘要
The Bekenstein-Hawking entropy, proportional to one quarter of the horizon area, is fundamental in black hole thermodynamics and can also be understood via the AdS/CFT correspondence, such as the 3D BTZ black hole and 2D CFT. In this work, we adopt the Kerr/CFT approach to analyze the central charge and black hole entropy for regular extremal black-bounce spacetimes, including the counterparts of the Kerr, Kerr-Newman, and Reissner-Nordström black holes. These spacetimes are free of curvature singularities at $r=0$. We derive the near horizon geometries of these spacetimes and find that they exhibit enhanced symmetry, namely SL$(2,\mathbb{R})\times \mathrm{U}(1)$ or SL$(2,\mathbb{R}) \times \mathrm{SO}(3)$. By imposing appropriate boundary conditions, we analyze their asymptotic symmetry groups, which contain diffeomorphisms as well as the $\mathrm{U}(1)_{\rm gauge}$ symmetry arising from the electromagnetic field. We then extract the central charge from the charge algebra and evaluate the left-moving temperature of the Frolov-Thorne vacuum. It is worth emphasizing that in the black-bounce Kerr-Newman case, the central charge from the electromagnetic contribution vanishes. Furthermore, in the black-bounce Reissner-Nordström case, we uplift the 4D geometry to a 5D configuration by incorporating a $\mathrm{U}(1)$ gauge fiber. Our results show that the microscopic entropy calculated from the Cardy formula is consistent with the Bekenstein-Hawking entropy. This agreement suggests that the Kerr/CFT approach remains valid for certain regular spacetimes without curvature singularities, thereby providing a microscopic statistical understanding of black hole entropy.
Comments26 pages, references added
