引力热量理论中具有锥形无穷远的黑洞

中文摘要 AI 辅助

引力热量理论是否允许施瓦西黑洞之外的球对称黑洞解，这一问题仍然悬而未决。一个定义良好的黑洞解需要同时具备正则视界和非奇异的外部区域，并且该外部区域延伸至无穷远。为了研究这个问题，我们将纯径向热量场的真空方程置于一般静态球对称度规中，转化为一个三维自治系统，这有助于对解进行全局分类。我们证明，正则渐近几何可以是闵可夫斯基几何或锥形几何，其中后者要求模型参数之间满足特定关系。在这一参数切片内，施瓦西黑洞是唯一渐近平坦的黑洞，而存在具有锥形无穷远的非施瓦西黑洞。这些黑洞从近视界区域到常规弱场区域（例如太阳系尺度）可以保持任意接近施瓦西黑洞，但在无穷远处却保留一个数量级为单位的立体角亏缺或盈余。渐近立体角仅依赖于一个模型参数，并且与热量场振幅无关。在固定的局部推断质量下，热量振幅决定了锥形转变尺度，较弱的场会使转变向外移动。我们推导了局部度规修正，并利用由此产生的近心点进动来构建对转变尺度的轨道测试。

英文摘要

Whether gravitational caloric theory admits spherical black-hole solutions beyond Schwarzschild remains open. A well-defined black-hole solution requires both a regular horizon and a nonsingular exterior extending to infinity. To investigate this question, we cast the vacuum equations for a purely radial caloric field in a general static spherically symmetric metric into a three-dimensional autonomous system, which facilitates the global classification of solutions. We show that the regular asymptotic geometry can be Minkowski or conical, with the latter requiring a specific relation between the model parameters. Within this parameter slice, Schwarzschild is the only asymptotically flat black hole, whereas non-Schwarzschild black holes with conical infinity exist. These black holes can remain arbitrarily close to Schwarzschild from the near-horizon region to the conventional weak-field region (e.g., Solar System scales), yet retain an order-unity solid-angle deficit or excess at infinity. The asymptotic solid angle depends on a single model parameter and is independent of the caloric field amplitude. At fixed locally inferred mass, the caloric amplitude sets the conical transition scale, with weaker fields shifting the transition outward. We derive the local metric corrections and use the resulting periapsis shift to formulate an orbital test of the transition scale.

发表机构

• Beijing Normal University（北京师范大学）
• Wuhan University（武汉大学）

机构由 AI 辅助整理，请以论文原文为准。

补充信息

备注

13 pages, 2 figures, submitted to Phys. Rev. D