In Poincaré gauge theory, black hole entropy is defined canonically by the variation of a boundary term ${\mathrm{\Gamma }}_H$, located at horizon. For a class of static and spherically symmetric black holes in vacuum, the explicit formula reads $\delta {\mathrm{\Gamma }}_H=T\delta S$, where T is black hole temperature and S entropy. Here, we analyze a new member of the same class, the Reissner-Nordström-like black hole with torsion [1], where the electric charge of matter is replaced by a gravitational parameter, induced by the existence of torsion. This parameter affects $\delta {\mathrm{\Gamma }}_H$ in a way that ensures the validity of the first law.

中文翻译：

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Reissner-Nordström 类黑洞的熵

在庞加莱规范理论中，黑洞熵由边界项的变化规范地定义 ${\mathrm{\Gamma }}_H$，位于地平线上。对于真空中一类静态和球对称黑洞，显式公式为$\delta {\mathrm{\Gamma }}_H=吨\delta 秒$，其中T是黑洞温度和S熵。在这里，我们分析了同一类的一个新成员，类似 Reissner-Nordström 的具有扭转的黑洞 [1]，其中物质的电荷被由扭转的存在引起的引力参数取代。该参数影响$\delta {\mathrm{\Gamma }}_H$ 以某种方式确保第一定律的有效性。