On Black Holes in Massive Gravity
On Black Holes in Massive Gravity
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DOI：
10.1103/physrevd.85.044024
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发表时间：
2011-11
影响因子：
5
通讯作者：
L. Berezhiani;G. Chkareuli;C. Rham;C. Rham;G. Gabadadze;A. Tolley
中科院分区：
文献类型：
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作者：
L. Berezhiani;G. Chkareuli;C. Rham;C. Rham;G. Gabadadze;A. Tolley
在大质量引力中，迄今为止在闵可夫斯基空间上发现的黑洞解恰好将视界转换为某种类型的奇点。在这里，我们探讨是否可以避免这些奇异性，如果时空不是渐近闵可夫斯基。我们找到了一个精确的解析黑洞（BH）的解决方案，通过在大尺度上过渡到自诱导的de Sitter（dS）时空，与引力子质量设置的曲率尺度，回避了上述问题。这个解类似于Koyama、Niz和Tasinato以及Nieuwenhuizen发现的解，但在细节上有所不同。结果表明，在Schwarzschild坐标系中，在有质量的GR中，BH度规必须伴随着具有非平凡背景的St“uckelberg场，以防止视界转化为奇点.我们还找到了dS空间上Reissner-Nordstr\“om BH的一个类似解。我们的方法的一个局限性是，我们只找到了理论的两个自由参数的特定值的解，对于这些值，矢量和标量波动都失去了它们的动力学项，然而，我们希望我们的解代表更广泛的一类，具有更好的表现扰动。
In massive gravity the so-far-found black hole solutions on Minkowski space happen to convert horizons into a certain type of singularities. Here we explore whether these singularities can be avoided if space-time is not asymptotically Minkowskian. We find an exact analytic black hole (BH) solution which evades the above problem by a transition at large scales to self-induced de Sitter (dS) space-time, with the curvature scale set by the graviton mass. This solution is similar to the ones discovered by Koyama, Niz and Tasinato, and by Nieuwenhuizen, but differs in detail. The solution demonstrates that in massive GR, in the Schwarzschild coordinate system, a BH metric has to be accompanied by the St\"uckelberg fields with nontrivial backgrounds to prevent the horizons to convert into the singularities. We also find an analogous solution for a Reissner-Nordstr\"om BH on dS space. A limitation of our approach, is that we find the solutions only for specific values of the two free parameters of the theory, for which both the vector and scalar fluctuations loose their kinetic terms, however, we hope our solutions represent a broader class with better behaved perturbations.