共查询到17条相似文献,搜索用时 109 毫秒
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避开求解黑洞背景下波动方程的困难,应用量子统计方法,直接求解轴对称Sen黑洞背景下Bose场和Fermi场的配分函数.然后利用改进的 brick-wall 方法-膜模型,计算黑洞背景下Bose场和Fermi场的熵.得到黑洞熵不但与黑洞的外视界面积有关,而且也是内视界面积的函数.在所得结论中不存在对数发散项与舍去项,也不存在黑洞视界外标量场或Dirac场为什么是黑洞熵疑难,并且给出粒子的自旋简并度对黑洞熵的影响. 当黑洞的辐射温度趋于绝对零度时,由黑洞内外视界面积决定的黑洞熵也趋于零,它满足能斯特定理,可视
关键词:
膜模型
黑洞熵
能斯特定理 相似文献
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避开求解黑洞背景下波动方程的困难,应用量子统计方法,直接求解轴对称KerrNewman黑洞背景下Bose场和Fermi场的配分函数.然后利用改进的brickwall方法膜模型,计算黑洞背景下Bose场和Fermi场的熵.得到黑洞熵与视界面积成正比的结论.在所得结论中不存在对数发散项与舍去项,也不存在黑洞视界外标量场或Dirac场为什么是黑洞熵疑难,并且给出粒子的自旋简并度对黑洞熵的影响.为研究各种复杂黑洞熵提供了简捷的途径.
关键词:
量子统计
brick-wall方法
膜模型
黑洞熵 相似文献
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在Tortoise坐标系中,利用brick-wall模型研究了来源于标量场的(2+1)维动态黑洞的量子熵.结果表明,在视界附近的薄区域内标量场的熵与黑洞熵有相同结构.特别是在静态情况下,量子熵满足熵的周长律.
关键词:
标量场
brick-wall模型
(2+1)维动态黑洞
量子熵 相似文献
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从Gibbons-Maeda(G-M)时空背景下的线元出发,利用WKB近似,由自旋为1/2的中微子场方程求得径向波数pkr,在此基础上利用brick-wall方法计算了G-M黑洞附近中微子场的自由能和熵,并与标量场的熵作了比较,发现中微子场的主项熵是标量场的主项熵的7/8倍. 相似文献
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计算了广义球对称含荷黑洞视界上标量场的量子态数和自由能,得到了黑洞熵与视界面积成 正比的结论,表明黑洞熵就是其视界上的量子态的熵.考虑广义不确定原理对黑洞熵的影响 ,采用二维膜模型,克服了brick-wall模型中的发散困难,计算中无须任何截断,且brick- wall模型中的小质量近似也可以避免.对视界外二维膜上的量子场的熵做了级数展开讨论, 得到了一些值得探讨的结论.
关键词:
广义不确定原理
黑洞熵
视界
截断 相似文献
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利用薄层(改进的brick-wall模型),通过分别求解标量场方程和Dirac场方程,计算了环面黑洞事件视界附近的标量场和Dirac场的量子统计熵.按薄层模型的观点,在视界面附近薄层上的量子场的熵就是黑洞的熵.结果表明,黑洞熵正比于事件视界的面积,遵循Beken-stein-Hawking面积熵公式.
关键词:
熵
环面黑洞
薄层模型
量子场 相似文献
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利用brick-wall方法计算了Anti-de Sitter时空内起源于Dirac场的柱黑洞的量子熵.结果表明,忽略远离围绕系统的真空的贡献时,量子熵包含了线性发散项和对数发散项,整个表达式的形式与标量场的不一样.无论整个对数项还是与自旋联系的子对数项都总是正的.
关键词:
brick-wall方法
量子熵
柱黑洞
Dirac场 相似文献
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The free energy and the entropy of scalar field are calculated by brick-wall in the axisymmetric Einstein–Maxwell–Dilaton-axion black hole. It is shown that when the black hole has inner and outer horizons, the entropy is not only related to the area of an outer horizon but also is the function of the area of an inner horizon. When the area of an inner horizon approaches zero, we can obtain the known conclusion. The entropy expressed by location parameter of outer horizon and inner horizons approaches absolute zero. It obeys Nernst theorem. It can be taken as Planck absolute entropy of a black hole. 相似文献
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ZHAORen WUYue-Qin ZHANGLi-Chun 《理论物理通讯》2003,40(6):745-748
In this paper, by using quantum statistical method, we obtain the partition function of Bose field and Fermi field on the background of the 5-dimensional rotating black hole. Then via the improved brick-wall method and membrane model, we calculate the entropy of Bose field and Fermi field of the black hole. And it is obtained that the entropy of the black hole is not only related to the area of the outer horizon but also is the function of inner horizon‘s area. In our results, there are not the left out term and the divergent logarithmic term in the original brick-wall method.The doubt that why the entropy of the scalar or Dirac field outside the event horizon is the entropy of the black hole in the original brick-wall method does not exist. The influence of spinning degeneracy of particles on entropy of the black hole is also given. It is shown that the entropy determined by the areas of the inner and outer horizons will approach zero,when the radiation temperature of the black hole approaches absolute zero. It satisfies Nernst theorem. The entropy can be taken as the Planck absolute entropy. We provide a way to study higher dimensional black hole. 相似文献
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In this paper, by using quantum statistical method, we obtain the partition function of Bose field and Fermi field on the background of the 5-dimensional rotating black hole. Then via the improved brick-wall method and membrane model, we calculate the entropy of Bose field and Fermi field of the black hole. And it is obtained that the entropy of the black hole is not only related to the area of the outer horizon but also is the function of inner horizon‘s area. In our results, there are not the left out term and the divergent logarithmic term in the original brick-wall method.The doubt that why the entropy of the scalar or Dirac field outside the event horizon is the entropy of the black hole in the original brick-wall method does not exist. The influence of spinning degeneracy of particles on entropy of the black hole is also given. It is shown that the entropy determined by the areas of the inner and outer horizons will approach zero,when the radiation temperature of the black hole approaches absolute zero. It satisfies Nernst theorem. The entropy can be taken as the Planck absolute entropy. We provide a way to study higher dimensional black hole. 相似文献
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We calculate the free energy and the entropy of a scalar field in terms of the brick-wall method on the background of the Reissner–Nordström black hole. We obtain the entropy of a scalar field is not only related to the location of an outer horizon but also is the function of the location of an inner horizon. In the approximation, the entropy is only proportional to the area of an outer horizon. The entropy expressed by location parameter of outer and inner horizon approaches zero, when the radiation temperature of a black hole approaches absolute zero. It satisfies the Nernst theorem. 相似文献
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Based on the 4-dimensional black hole solution of $f(R)$ theory coupled to a nonlinear Maxwell field, we calculate the interior volume of a charged $f(R)$ black hole using the method proposed by Christodoulou and Rovelli. Considering massless scalar field in the interior volume and Hawking radiation carrying only energy, we calculate the entropy of the scalar field inside a charged $f(R)$ black hole and investigate the evolution of the entropy under Hawking radiation. In the meantime, the evolution of the Bekenstein-Hawking entropy under Hawking radiation has also been calculated. Based on these results, the proportional relation is obtained between the evolution of the scalar field entropy and the evolution of Bekenstein-Hawking entropy under Hawking radiation. According to the result, we investigate and discuss how the modified coefficient $b$ in $f(R)$ gravity theory affects the evolution relation between the two types of entropy. It is shown that the radiation rate for Hawking radiation of a charged $f(R)$ black hole can increase with the modified coefficient $b$. 相似文献