Flux-area operator and black hole entropy
Flux-area operator and black hole entropy
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DOI：
10.1103/physrevd.80.044016
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发表时间：
2009-05
影响因子：
5
通讯作者：
G. J.FernandoBarbero;J. Lewandowski;Eduardo J S Villaseñor
中科院分区：
文献类型：
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作者：
G. J.FernandoBarbero;J. Lewandowski;Eduardo J S Villaseñor
我们证明，对于具有内边界的时空，存在一个不同于环量子引力中使用的标准面积算子的自然面积算子。这个新的通量面积算子具有等距特征值。我们讨论了用新的黑洞熵定义替换Ashtekar-Baez-Corichi-Krasnov定义中的标准面积算子的结果。我们的选择简化了熵的定义，并允许我们只考虑那些与描述视界自由度的chen - simons理论的水平值所定义的值一致的区域。给出了用自旋分量计算相关视界态个数的公式，并得到了黑洞熵的精确表达式。最后我们推导了它的渐近性，讨论了我们的结果与Bekenstein-Hawking面积定律的相容性以及与Schwarzschild拟正态模的关系。
We show that, for space-times with inner boundaries, there exists a natural area operator different from the standard one used in loop quantum gravity. This new flux-area operator has equidistant eigenvalues. We discuss the consequences of substituting the standard area operator in the Ashtekar-Baez-Corichi-Krasnov definition of black hole entropy by the new one. Our choice simplifies the definition of the entropy and allows us to consider only those areas that coincide with the one defined by the value of the level of the Chern-Simons theory describing the horizon degrees of freedom. We give a prescription to count the number of relevant horizon states by using spin components and obtain exact expressions for the black hole entropy. Finally we derive its asymptotic behavior, discuss several issues related to the compatibility of our results with the Bekenstein-Hawking area law and the relation with Schwarzschild quasinormal modes.