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 共查询到17条相似文献,搜索用时 78 毫秒
1.
动态广义球对称含荷黑洞Dirac场的熵   总被引:1,自引:0,他引:1       下载免费PDF全文
郑元强 《物理学报》2006,55(7):3272-3276
利用改进后的薄膜brick-wall模型,计算了动态广义球对称含荷黑洞Dirac场的熵.按薄层模型的观点,在视界附近薄场上的熵就是黑洞的熵.计算结果表明所得到的黑洞熵与其视界面积成正比. 关键词: 黑洞 薄膜brick-wall模型 熵 Dirac场  相似文献   

2.
一般球对称带电蒸发黑洞Dirac场的熵   总被引:8,自引:1,他引:7       下载免费PDF全文
张靖仪 《物理学报》2003,52(9):2354-2358
采用薄层模型brick-wall方法,计算了一般球对称带电蒸发黑洞Dirac场的熵,通过适当选择时间依赖的截断因子,仍可得出黑洞熵与视界面积成正比的结论. 关键词: 熵 蒸发黑洞 薄层模型 Dirac场 Dirac方程  相似文献   

3.
动态黑洞的瞬时辐出度   总被引:7,自引:0,他引:7       下载免费PDF全文
孟庆苗 《物理学报》2005,54(1):471-474
选取超前爱丁顿坐标,采用统计的方法,计算出动态黑洞的瞬时辐出度.结果表明,动态黑洞的瞬时辐出度不仅与假定黑洞处于热力学平衡时的辐出度有关,还与黑洞的事件视界变化率、事件视界温度、事件视界附近的熵密度及黑洞的吸收和辐射系数有关.对于球对称动态黑洞,任一时刻黑洞的瞬时辐出度总是正比于黑洞事件视界温度的四次方. 关键词: 熵密度 事件视界温度 薄膜模型 瞬时辐出度  相似文献   

4.
王波波 《物理学报》2004,53(7):2401-2406
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   

5.
静态球对称黑洞Dirac场的Stefan-Boltzmann定律   总被引:27,自引:1,他引:26       下载免费PDF全文
孟庆苗 《物理学报》2003,52(8):2102-2104
利用静态球对称黑洞Dirac场的统计熵,导出静态球对称黑洞的Stefan-Boltzmann定律,得 到黑洞的辐出度与视界温度的四次方成正比的结论.发现Stefan-Boltzmann常数不同于平直 时空的值,并且在不同时空度规中该常数有不同的值. 关键词: 黑洞 统计熵 薄层模型 辐出度  相似文献   

6.
动态广义球对称含荷黑洞的统计熵   总被引:9,自引:1,他引:8       下载免费PDF全文
利用改进了的brickwall膜模型,计算了动态广义球对称含荷黑洞的熵,研究结果表明,对于动态黑洞,将黑洞熵表示为与视界面积成正比时,则比例系数总与动态黑洞的视界速度有关 关键词: 广义球对称黑洞 黑洞熵 brick-wall膜模型 WKB近似  相似文献   

7.
杨学军  赵峥 《物理学报》2011,60(6):60401-060401
计算黑洞熵的砖墙模型被改进为薄膜模型后其物理思想更直接而明了,且突出了事件视界作为静态或稳态黑洞特征面的重要性.但为避免发散,薄膜模型同样需要引入紫外截断因子.截断因子的引入非常人为,至今没有给以合理的解释.有文献将广义不确定关系引入黑洞熵的计算而不需要任何截断便可避免发散.本文以静态球对称黑洞Dirac场的熵的计算为例,阐述了无截断薄膜模型及其与有截断薄膜模型的本质区别. 关键词: 黑洞熵 无截断薄膜模型 广义不确定关系 Dirac场  相似文献   

8.
高自旋场对静态球对称黑洞熵的贡献   总被引:10,自引:0,他引:10       下载免费PDF全文
苏九清  李传安 《物理学报》2005,54(2):530-533
利用改进后的brick wall模型,研究具有高自旋的引力场对静态球对称黑洞熵的贡献.结果表明:在静态球对称黑洞中,自旋为2的引力场的量子熵仍与视界面积成正比.当选择与标量场相同的截断因子时,其量子熵为标量场的两倍,为Dirac场的4/7. 关键词: 黑洞熵 brick wall模型 自旋场 Teukolsky型主方程  相似文献   

9.
将广义不确定关系引入新的态密度方程,采用WKB近似方法,对含整体单极黑洞Dirac场的熵进行了直接计算,所得黑洞熵与它的视界面积成正比,以此揭示了黑洞熵是其视界面处量子态的熵.与brick-wall模型方法不同,该结果不需要取任何截断.同时表明,用此方法不仅可以计算黑洞标量场的熵,而且可以计算Dirac场的熵.  相似文献   

10.
静态球对称黑洞Dirac场的统计熵   总被引:37,自引:3,他引:34       下载免费PDF全文
李传安  孟庆苗  苏九清 《物理学报》2002,51(8):1897-1900
利用改进的brickwall模型,给出了一类静态球对称黑洞Dirac场的熵,结果表明,在取相同的截断因子时,Dirac场的熵均为标量场的熵的72倍 关键词: 黑洞 统计熵 brickwall模型 Dirac场  相似文献   

11.
郑元强 《物理学报》2007,56(3):1266-1270
采用新的广义乌龟坐标变换,利用薄膜brick-wall模型.讨论了球对称动态黑洞Driac场的Hawking温度和熵,由于k因子的变化,使Hawking温度有一定影响,而截断因子不再因时空结构不同而异,变得与稳态情况相同. 关键词: 广义乌龟坐标变换 薄膜brick-wall模型 Driac场 熵  相似文献   

12.
By using the method of quantum statistics, we derive directly the partition functions of bosonic andfermionic fields in the N-dimensional spherically symmetric charged black hole space-time. The statistical entropy ofblack hole is obtained by an improved brick-wall method. When we choose proper parameters in our results, we canobtain that the entropy of black hole is proportional to the area of horizon. In our result, there do not exist neglectedterm and divergent logarithmic term given in the original brick-wall method. We avoid the difficulty in solving the waveequation of scalar and Dirac fields. We offer a simple and direct way of studying entropy of the higher-dimensional black hole.  相似文献   

13.
孟庆苗  蒋继建  李中让  王帅 《中国物理 B》2010,19(9):90402-090402
By the statistical entropy of the Dirac field of the static spherically symmetric black hole, the result is obtained that the radiation energy flux of the black hole is proportional to the quartic of the temperature of its event horizon. That is, the thermal radiation of the black hole always satisfies the generalised Stenfan-Boltzmann law. The derived generalised Stenfan-Boltzmann coefficient is no longer a constant. When the cut-off distance and the thin film thickness are both fixed, it is a proportional coefficient related to the space-time metric near the event horizon and the average radial effusion velocity of the radiation particles from the thin film. Finally, the radiation energy fluxes and the radiation powers of the Schwarzschild black hole and the Reissner-Nordstrm black hole are derived, separately.  相似文献   

14.
The geometry of the neighborhood near an event horizon is similar to the Rindlermetric, which leads to the thermal effect of black holes. The entropy of the scalarfield and the Dirac field are calculated in the black-hole background. The entropyof the scalar field, which is proportional to the area of the event horizon, isnaturally derived. Under the condition of large-mass black hole, the entropy ofthe Dirac field is still proportional to the area of the horizon. These results canbe applied to a large class of black holes. A new method for calculating the blackhole entropy is proposed which makes it easy to calculate the entropy of ahigh-spin field in the black-hole background. We also consider extreme black holesand point out that the topological entropy only has classical meaning.  相似文献   

15.
By using the method of quantum statistics, we derive directly the partition functions of bosonic and fermionic field in the black hole space-time with different temperatures on horizon surface. The statistical entropy of the black hole is obtained by an improved brick-wall method. When we choose a proper parameter in our results, we can obtain that the entropy of the black hole is proportional to the area of horizon. In our result, there do not exist any neglected term or divergent logarithmic term as given in the original brick-wall method. We have avoided the difficulty in solving the wave equation of the scalar and Dirac field. A simple and direct way of studying entropy of the black hole is given.  相似文献   

16.
By using the method of quantum statistics, we derive directly the partition functions of bosonic and fermionic field in the d-dimensional Horowitz-Strominger black hole. The statistical entropy of black hole is obtained by an improved brick—wall method. When we choose proper parameter in our results, we can obtain that the entropy of the black hole is proportional to the area of the horizon. In our result, there don't exist the left out term and divergent logarithmic term given in the original brick—wall method. We avoid the difficulty in solving the wave equation of scalar and Dirac field. And we offer a simple and direct way of studying entropy of the higher-dimensional complicated black hole.  相似文献   

17.
Using entropy density of Dirac field near the event horizon of a rectilinear non-uniformly accelerating Kinnersley black hole, the law for the thermal radiation of black hole is studied and the instantaneous radiation energy density is obtained. It is found that the instantaneous radiation energy density of a black hole is always proportional to the quartic of the temperature on event horizon in the same direction. That is to say, the thermal radiation of a black hole always satisfies the generalized Stefan-Boltzmann law. In addition, the derived generalized Stefan-Boltzmann coefficient is no longer a constant, but a dynamic coefficient related to the space-time metric near the event horizon and the changing rate of the event horizon in black holes.  相似文献   

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