带有电荷、磁荷的一类任意加速黑洞的瞬时辐射能通量

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.     

The thermal radiation from dynamic black holes

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)     

动态Dilaton-Maxwell黑洞的广义Stefan-Boltzmann定律

利用动态Dilaton-Maxwell黑洞视界面附近的熵密度,导出黑洞的瞬时辐射流量,得到了任一时刻黑洞沿某一方向的瞬时辐射流量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面附近的时空度规、黑洞视界的变化率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： 熵密度 薄膜模型 瞬时辐射流量 广义Stefan-Boltzmann系数     

The Generalized Stefan-Boltzmann Law of Slowly Changing Kerr-Newman Black Hole

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.     

加速运动动态黑洞的瞬时辐出度

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     

Radiation Energy Flux and Radiation Power of Schwarzschild Black Hole

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.     

Instantaneous Radiation Energy Flux and Radiation Power Near the Event Horizon of Slowly Changing Vaidya Black Hole

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.     

Barriola-Vilenkin黑洞Dirac场的广义Stefan-Boltzmann定律

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。     

球对称动态黑洞视界附近的瞬时辐射能通量及瞬时辐射功率

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.     

Radiation energy flux of Dirac field of static spherically symmetric black holes

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--Nordstrõm black hole are derived, separately.     

动态黑洞的瞬时辐出度

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     

Thermal radiation and nonthermal radiation of the slowly changing dynamic Kerr--Newman black hole

Using the related formula of dynamic black hole, we have calculated the instantaneous radiation energy density of the slowly changing dynamic Kerr-Newman black hole. It is found that the instantaneous radiation energy density of a black hole is always proportional to the quartic of the temperature of the event horizon in the same direction. By using the Hamilton-Jacobin equation of scalar particles in the curved spacetime, the spontaneous radiation of the slowly changing dynamic Kerr-Newman black hole is studied. The energy condition for the occurrence of the spontaneous radiation is obtained.     

The Thermal Radiation from Static Spherically Symmetric Black Holes

By use of the radiant emittance near the event horizon of static spherically symmetric black hole, the radiation field around the black hole was studied and found the generalized Stefan Boltzmann coefficient σ of thermal radiation near the event horizon is much greater than the flat space-time blackbody radiation. For Schwarzschild black hole, σ will increased as the black hole mass increases. For Reissner-Nordström black hole, σ has some relation with the quality and the charges of the black hole. Thermal particle model was proposed creatively to study the radiation power and radiant energy flux of static spherically symmetric black hole, found when η take the inherent thickness, for all Schwarzschild black hole the radiation power are the same and the radiant energy flux is inversely proportional to the square of the distance from observer to the black hole, for Reissner-Nordström black hole the radiation power is associated with the quality and the charge of the black hole. When given the mass and charges of the black hole, the radiant energy flux is inversely proportional to the square of the distance from observer to the black hole.     

Quantum Entropy of Black Hole with Internal Global Monopole

Using the generalized uncertainty relation, the new equation of state density is obtained, and then the entropy of black hole with an internal global monopole is discussed. The divergence that appears in black hole entropy calculation through original brick-wall model is overcome. The result of the direct proportion between black hole entropy and its event horizon area is drawn and given. The result shows that the black hole entropy must be the entropy of quantum state near the event horizon.     

Schwarzschild-de Sitter黑洞宇宙视界量子态的熵

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     

Schwarzschild-de-Sitter黑洞宇宙视界量子态的熵

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     

Thermodynamical quantities around a RNAdS black hole

The entropy density, energy density, pressure and equation of state around the RNAdS black hole are calculated in the WKB approximation on the Teukolsky-type master equation. The appearance of spin-dependent terms is demonstrated. The existence of these terms shows that the black hole radiation is not exactly thermal radiation and the black hole entropy is not strictly proportional to the area of the event horizon.     

The Generalized Uncertainty Relation and The Entropy of Non-stationary and Slowly Changing Reissner-Nordstr?m Black Hole

Applying the generalized uncertainty relation to the thin film brick-wall model, the entropy of Dirac Field in Non-stationary and Slowly Changing Reissner-Nordstr?m Black Hole is obtained. The result shows that the entropy is still proportional to the horizon area of the black hole, and black hole entropy is just identical to the entropy of the quantum state near the event horizon, in addition, the divergence of state density without any cut-off parameter is avoided during black hole entropy calculation.     

Kerr-Newman-de Sitter黑洞辐射谱和熵修正

本文延拓Damour-Ruffini方法,研究Kerr-Newman-de Sitter黑洞的Hawking辐射.在保持时空中总能量,总角动量和总电荷守恒的条件下,考虑辐射粒子对时空的反作用与黑洞事件视界和宇宙视界的相互关联后,得到了黑洞辐射谱.此辐射不再是严格的纯热谱与黑洞事件视界和宇宙视界对应Bekenstein-Hawking熵变有关.研究发现其结果仍然符合幺正性原理.同时给出了黑洞Bekenstein-Hawking熵的修正项.使人们对黑洞热辐射的研究有了进一步的认识.     

Schwarzschild-de Sitter黑洞的Hawking辐射

利用延拓Damour-Ruffini方法,研究Schwarzschild-de Sitter黑洞的Hawking辐射.在保持时空中总能量守恒的条件下,考虑辐射粒子对时空的反作用和黑洞事件视界与宇宙视界的相互关联后,得到黑洞辐射谱.此辐射不再是严格的纯热谱,与黑洞事件视界和宇宙视界对应Bekenstein-Hawking熵变有关,发现其结果仍然符合幺正性原理. 关键词： Damour-Ruffini方法 Hawking辐射 能量守恒