【摘要】 引入局域热平衡概念 ,用Damour Ruffini方法和薄膜模型研究了缓变动态Kerr Newman黑洞的Hawking辐射和熵 .得到了黑洞的Hawking温度和辐射谱公式 ,Hawking温度随时间和视界面上的位置而变化 ,辐射谱为准黑体谱 ;计算了黑洞熵 ,当取与静态球对称黑洞情况相同的截断关系时便得到了黑洞的Bekenstein Hawking熵 .结果表明 ,缓变动态黑洞的温度是局域量 ,缓变动态黑洞的熵与稳态黑洞情况一样正比于黑洞视界面面积更多还原

【Abstract】 Introducing the notion of the local thermal equilibrium,the Hawking effect and the entropy of a nonstationary Kerr Newman black hole whose metric changes slowly are studied by the method of Damour Ruffini and the thin film model.First,we obtain the Hawking radiation temperature and the thermal spectrum formula,and show that the Hawking temperature depends on the time and the location on the event horizon,the thermal spectrum is a quasi black body’s thermal spectrum.Second,we calculate the black hole entropy,which is just the Bekenstein Hawking entropy with the same geometrical cutoff relationship as in the static and spherical case.The results show that the temperature of the black hole is a local quantity,and the entropy of the non stationary black hole is also proportional to the horizon area as in the case of stationary black holes.更多还原