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 共查询到17条相似文献,搜索用时 109 毫秒
1.
孟庆苗  苏九清  蒋继建 《物理学报》2007,56(9):5077-5082
利用加速黑洞视界面附近的熵密度,导出黑洞的瞬时辐出度,得到了任一时刻黑洞沿某一方向的瞬时辐出度总是正比于在该方向上黑洞事件视界温度的四次方的结论. 导出的广义Stefan-Boltzmann系数不再是一个恒量,而是一个与黑洞视界的变化率、黑洞视界面附近的时空度规及黑洞的吸收与辐射系数有关的动比例系数. 揭示了黑洞周围的引力场与其热辐射之间存在着必然的内在联系. 关键词: 薄膜模型 瞬时辐出度 广义Stefan-Boltzmann系数  相似文献   

2.
利用带有电荷、磁荷的一类任意加速黑洞视界面附近标量场的熵密度,研究黑洞的热辐射规律,导出了黑洞的瞬时辐射能通量,得到了黑洞的热辐射总是满足广义Stefan-Boltzmann定律的结论.导出的广义Stefan-Boltzmann系数不是常数,而是一个与黑洞参量(质量、所带的电荷与磁荷、加速度的大小、视界的变化率)有关的动比例系数.对于不同的动态黑洞,由于黑洞周围的引力场和电磁场不同,导出的广义Stefan-Boltzmann系数也不同.  相似文献   

3.
孟庆苗  李中让  李玉山 《物理学报》2010,59(10):6847-6850
利用薄膜模型研究Barriola-Vilenkin黑洞的热辐射,得到了黑洞的热辐射满足广义Stefan-Boltzmann定律的结论,导出的广义Stefan-Boltzmann系数不再是一个恒量,当截断距离以及薄膜厚度取定后,它是一个与黑洞视界附近的时空度规以及辐射粒子的径向平均泻流速率有关的比例系数.得到的Barriola-Vilenkin黑洞视界附近Dirac场的辐射能通量与薄层膜内辐射粒子的径向平均泻流速率成正比,与黑洞的质量平方成反比。  相似文献   

4.
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   

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.
Schwarzschild-de-Sitter黑洞宇宙视界量子态的熵   总被引:1,自引:0,他引:1       下载免费PDF全文
韩亦文  洪云 《物理学报》2004,53(10):3270-3273
采用由广义不确定关系得到的新的态密度方程,研究了Schwarzchild-de-Sitter时空背景下黑洞宇宙视界的熵.利用新的态密度方程,克服了用brick wall模型方法计算黑洞熵,在消除紫外发散需取截断的不完善之处,以此揭示了黑洞熵与其视界面积成正比这一内在联系,进一步表明黑洞熵是视界面处量子态的熵. 关键词: 黑洞 广义不确定关系 态密度 熵  相似文献   

7.
杨波 《物理学报》2008,57(4):2614-2620
在一般加速带电带磁的动态黑洞中,化简Klein-Gordon场方程,利用乌龟坐标变换,得到在视界面附近的辐射温度.用薄膜brick-wall模型,选择适当的截断因子和薄膜厚度,得到在视界面附近薄膜上的熵,结果表明黑洞熵与视界面积成正比. 关键词: 黑洞 Hawking温度 薄膜brick-wall模型 熵  相似文献   

8.
刘成周  赵峥 《物理学报》2006,55(4):1607-1615
按纠缠熵方法,计算了Gibbons-Maeda(G-M)dilaton黑洞视界外部与黑洞内量子态纠缠的一薄层内量子场的统计熵,得到了G-M dilaton黑洞的Bekenstein-Hawking熵.用广义不确定原理对量子态密度进行修正,克服了brick-wall模型中视界附近态密度的发散困难,该薄层可以紧贴在事件视界上.对brick-wall外部量子场中与黑洞内自由度有关联的自由度统计熵进行了计算,并把结果与brick-wall内量子场的熵进行比较分析,显示两结果具有与视界面积成正比的一致性,但后者能更 关键词: 纠缠熵 黑洞 广义不确定原理 截断  相似文献   

9.
采用由广义不确定关系得到的新的态密度方程 ,研究了Schwarzchild deSitter时空背景下黑洞宇宙视界的熵 .利用新的态密度方程 ,克服了用brick wall模型方法计算黑洞熵 ,在消除紫外发散需取截断的不完善之处 ,以此揭示了黑洞熵与其视界面积成正比这一内在联系 ,进一步表明黑洞熵是视界面处量子态的熵  相似文献   

10.
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   

11.
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   

12.
Using the related formula of dynamic black holes, the instantaneous radiation energy density of the general spherically symmetric charged dynamic black hole and the arbitrarily accelerating charged dynamic black hole is calculated. It is found that the instantaneous radiation energy density of black hole is always proportional to the quartic of the temperature of event horizon in the same direction. The proportional coefficient of generalized Stefan-Boltzmann is no longer a constant, and it becomes a dynamic coefficient that is related to the event horizon changing rate, space-time structure near event horizon and the radiation absorption coefficient of the black hole. It is shown that there should be an internal relation between the gravitational field around black hole and its thermal radiation. Supported by the Science Foundation of Heze University (Grant No. XY06WL01)  相似文献   

13.
孟庆苗  蒋继建  李传安 《物理学报》2010,59(3):1481-1486
采用黑洞的薄膜模型和局域热平衡的假定,研究球对称动态黑洞视界附近的瞬时辐射能通量和瞬时辐射功率,得到了当截断距离η取定后,Vaidya黑洞视界附近标量场的瞬时辐射能通量与黑洞的质量和视界变化率有关,其瞬时辐射功率仅与黑洞的视界变化率有关.Vaidya-Bonner黑洞的瞬时辐射能通量和瞬时辐射功率与黑洞的质量、电荷和视界变化率有关.表明黑洞周围的引力场、电磁场以及视界的变化均对黑洞的热辐射产生影响.  相似文献   

14.
Using the entropy density near the event horizon of Kerr-Newman black hole, the instantaneous radiation energy flux and the instantaneous radiation power of the slowly changing Kerr-Newman black hole have been studied. It is found that the thermal radiation of the Kerr-Newman black hole always satisfies the generalized Stefan-Boltzmann law and is affected by the gravitational field, the electromagnetic field around the black hole and the change of black hole event horizon. But the rate of the change of the event horizon usually makes very little affect on the instantaneous radiation energy flux and radiation power. Only when the rate of the change of the event horizon approaches to the light speed, it can make obviously affect on them.  相似文献   

15.
By the thin film model of the black hole and the assumption of the local thermal equilibrium, the instantaneous radiation energy flux and radiation power of the slowly changing Vaidya black hole have been studied. The result has been obtained that the thermal radiation of the Vaidya black hole satisfies the generalized Stefan-Boltzmann law. When the cut-off distance and the thin film thickness are both fixed, the instantaneous radiation energy flux of the scalar field near the event horizon of the Vaidya black hole is not only related to the black hole mass, but also to the rate of the change of its event horizon and the average effusion velocity of the radiation particles in the thin film. While its instantaneous radiation power is related to the rate of the change of the event horizon and the average radial effusion velocity of the radiation particles in the thin film. These results indicate that the gravitational field around the black hole and the change of its event horizon will both affect the thermal radiation of the black hole.  相似文献   

16.
Applying the entropy density near the event horizon, we obtained the result that the radiation energy flux of the black hole is always proportional to the quartic of the temperature of its event horizon. That is to say, the thermal radiation of the black hole always satisfies the generalized Stefan–Boltzmann law. The derived generalized Stefan–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 which is related to the black hole mass, the kinds of radiation particles and space–time metric near the event horizon. In this paper, we have put forward a thermal particle model in curved space–time. By this model, the result has been obtained that when the thin film thickness and the cut-off distance are both fixed, the radiation energy flux received by observer far away from the Schwarzschild black hole is proportional to the average radial effusion velocity of the radiation particles in the thin film, and inversely proportional to the square of the distance between the observer and the black hole.  相似文献   

17.
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   

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