黑洞熵：深入探究
Black Hole Entropy: A Closer Look.
作者信息
Tsallis Constantino
机构信息
Centro Brasileiro de Pesquisas Físicas and National Institute of Science and Technology of Complex Systems, Rua Xavier Sigaud 150, Rio de Janeiro 22290-180, RJ, Brazil.
Santa Fe Institute, 1399 Hyde Park Road, Santa Fe, NM 87501, USA.
出版信息
Entropy (Basel). 2019 Dec 22;22(1):17. doi: 10.3390/e22010017.
In many papers in the literature, author(s) express their perplexity concerning the fact that the ( 3 + 1 ) black-hole 'thermodynamical' entropy appears to be proportional to its area and not to its volume, and would therefore seemingly be nonextensive, or, to be more precise, subextensive. To discuss this question on more clear terms, a non-Boltzmannian entropic functional noted S δ was applied [Tsallis and Cirto, Eur. Phys. J. C 73, 2487 (2013)] to this complex system which exhibits the so-called area-law. However, some nontrivial physical points still remain open, which we revisit now. This discussion is also based on the fact that the well known Bekenstein-Hawking entropy can be expressed as being proportional to the event horizon area divided by the square of the Planck length.
在文献中的许多论文里，作者们对这样一个事实表示困惑：（3 + 1）维黑洞的“热力学”熵似乎与其面积成正比，而非与其体积成正比，因此表面上似乎是非广延的，或者更确切地说，是次广延的。为了更清晰地讨论这个问题，一个名为(S_{\delta})的非玻尔兹曼熵泛函[Tsallis和Cirto，《欧洲物理杂志C》73，2487（2013）]被应用于这个呈现所谓面积律的复杂系统。然而，一些重要的物理问题仍然悬而未决，我们现在重新审视这些问题。这个讨论也是基于这样一个事实：著名的贝肯斯坦 - 霍金熵可以表示为与事件视界面积除以普朗克长度的平方成正比。
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