arXiv 2212.094952022-12-19gr-qcastro-ph.HE

渐近安全引力及更远引力中的黑洞

Black holes in asymptotically safe gravity and beyond

Astrid Eichhorn, Aaron Held

备注：: invited chapter for the book ''Regular Black Holes: Towards a New Paradigm of the Gravitational Collapse''; comments welcome

摘要：

渐近安全量子引力是量子引力的一种方法，它为度规建立了一个标准的量子场论。因此，即使是被期望确定黑洞核心真实结构的深量子引力体系，也是由时空度规描述的。渐近安全的本质在于理论的一种新的对称性--量子尺度对称性--它表征了量子引力的短距离区域。这意味着没有物理尺度。因此，牛顿耦合，这对应于一个尺度，即普朗克长度，必须在短距离制度渐近消失。这意味着引力相互作用的减弱，由此可以期望经典时空奇点的解析。在实践中，黑洞在渐近安全量子引力中的性质还不能从第一性原理推导出来，而是使用一种称为重整化群改进的启发式过程来构造。由此产生的渐近安全启发黑洞已被构造为零和非零自旋参数。它们的特点是：（i）曲率奇点的情况下，（ii）一个更紧凑的事件视界和光子球，（iii）第二（内）地平线，即使在消失的自旋和（iv）冷残余作为一个可能的最终产品的霍金蒸发。观测可以开始限制量子引力尺度，在渐近安全启发的黑洞中，量子引力尺度可以被视为自由参数。对于缓慢旋转的黑洞，来自EHT和X射线观测的约束只能约束远远超过普朗克长度的量子引力尺度。在近临界自旋的极限，渐近安全启发的黑洞可能"点亮”的方式ngEHT可能是敏感的，即使是量子引力尺度等于普朗克长度。

英文摘要：

Asymptotically safe quantum gravity is an approach to quantum gravity that achieves formulates a standard quantum field theory for the metric. Therefore, even the deep quantum gravity regime, that is expected to determine the true structure of the core of black holes, is described by a spacetime metric. The essence of asymptotic safety lies in a new symmetry of the theory -- quantum scale symmetry -- which characterizes the short-distance regime of quantum gravity. It implies the absence of physical scales. Therefore, the Newton coupling, which corresponds to a scale, namely the Planck length, must vanish asymptotically in the short-distance regime. This implies a weakening of the gravitational interaction, from which a resolution of classical spacetime singularities can be expected. In practise, properties of black holes in asymptotically safe quantum gravity cannot yet be derived from first principles, but are constructed using a heuristic procedure known as Renormalization Group improvement. The resulting asymptotic-safety inspired black holes have been constructed both for vanishing and for nonvanishing spin parameter. They are characterized by (i) the absence of curvature singularities, (ii) a more compact event horizon and photon sphere, (iii) a second (inner) horizon even at vanishing spin and (iv) a cold remnant as a possible final product of the Hawking evaporation. Observations can start to constrain the quantum-gravity scale that can be treated as a free parameter in asymptotic-safety inspired black holes. For slowly-spinning black holes, constraints from the EHT and X-ray observations can only constrain quantum-gravity scales far above the Planck length. In the limit of near-critical spin, asymptotic-safety inspired black holes may ``light up" in a way the ngEHT may be sensitive to, even for a quantum-gravity scale equalling the Planck length.

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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