共查询到20条相似文献,搜索用时 46 毫秒
1.
Xin-Qin Gao Li-E Qiang Jian-Yang Zhu Zheng Zhao 《General Relativity and Gravitation》2004,36(11):2511-2523
By reducing the Klein-Gordon equation near the event horizon with a new tortoise coordinate transformation, we calculate the Hawking temperature of the arbitrarily accelerating Kinnersley black hole. The temperature is a little different from what we have when we select the usual tortoise coordinate transformation. Then by means of the thin film model, we obtain the Bekenstein Hawking entropy of the Kinnersley black hole, which is proportional to the area of its event horizon with the same cut-off relation as the static case. 相似文献
2.
Zhao Zheng Zhang Jian-hua Zhu Jian-yang 《International Journal of Theoretical Physics》1995,34(10):2039-2048
The Hawking radiation of an arbitrarily accelerating Kinnersley black hole is studied. We obtain the event horizon equation and the Hawking thermal spectrum formula. Both the location and the temperature of the event horizon depend on the time and the angles. We recover the well-known results when the acceleration vanishes. 相似文献
3.
The Hawking radiation of Dirac particles in an arbitrarily rectilinearly accelerating Kinnersley black hole with electromagnetic charge and cosmological constant is investigated by using the generalized tortoise coordinate transformation. Both the location and the temperature of the event horizon depend on the time and the polar angle. The Hawking thermal radiation spectrum of Dirac particles is also derived. 相似文献
4.
Hawking radiation of Weyl neutrinos in a rectilinearly non—uniformly accelerating Kinnersley black hole 下载免费PDF全文
The quantum thermal effect of Weyl neutrinos in a rectilinearly non-uniformly accelerating Kinnersley black hole is investigated using the generalized tortoise coordinate transformation.The equations that determine the location,the Hawking temperature of the event horizon and the thermal radiation spectrum of neutrinos are derived.Our results show that the location and the temperature of the event horizon depend not only on the time but also on the angle. 相似文献
5.
6.
Hawking Radiation of Dirac Particles in an Arbitrarily Accelerating Kinnersley Black Hole 总被引:1,自引:0,他引:1
Quantum thermal effect of Dirac particles in an arbitrarily accelerating Kinnersley black hole is investigated by using the method of generalized tortoise coordinate transformation. Both the location and the temperature of the event horizon depend on the advanced time and the angles. The Hawking thermal radiation spectrum of Dirac particles contains a new term which represents the interaction between particles with spin and black holes with acceleration. This spin-acceleration coupling effect is absent from the thermal radiation spectrum of scalar particles. 相似文献
7.
采用Tortoise坐标变换,约化视界面附近Dirac场方程,得到Kinnersley黑洞的Hawking温度.用薄膜brick-wall模型,计算Kinnersley黑洞的熵,得到通过选择适当的截断因子和薄层,在视界面附近薄层上的熵就是黑洞的熵,结果表明黑洞熵与视界面积成正比. 相似文献
8.
采用两种新的乌龟坐标变换,用改进的Damour-Ruffini方法研究了动态Kinnersley黑洞的Hawking辐射.在新乌龟坐标变换下,将Klein-Gordon方程在视界附近变换成平直时空的标准波动方程形式,得到了黑洞的表面引力及Hawking温度,该温度在黑洞表面不同点有不同的值.值得注意的是,旧的乌龟坐标变换存在量纲错误,新乌龟坐标变换没有量纲问题,选不同的旧乌龟坐标变换计算同一黑洞所得结果不同,但是采用不同的新乌龟坐标变换所得结果仍然不同.
关键词:
黑洞
乌龟坐标变换
Hawking辐射
Klein-Gorden方程 相似文献
9.
Kinnersley has discussed the space–time of an arbitrarily accelerating point mass. We select a simple case in which the black hole is uniformly accelerated and the mass does not vary with time. We adopt thin film brick-wall model to calculate the entropy of black hole. We find that both the temperature and the entropy density of black hole can be calculated at every point on the horizon. This result indicates that the conclusion that black hole entropy is proportional to its area can be applied to horizon not only globally, but also locally. 相似文献
10.
11.
The generalized Stefan--Boltzmann law of a rectilinear non-uniformly accelerating Kinnersley black hole 下载免费PDF全文
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.
Hawking effect and quantum nonthermal radiation of an arbitrarily accelerating charged black hole using a new tortoise coordinate transformation 下载免费PDF全文
Using a new tortoise coordinate transformation, this paper investigates the Hawking effect from an arbitrarily accelerating charged black hole by the improved Damour-Ruffini method. After the tortoise coordinate transformation, the Klein-Gordon equation can be written as the standard form at the event horizon. Then extending the outgoing wave from outside to inside of the horizon analytically, the surface gravity and Hawking temperature can be obtained automatically. It is found that the Hawking temperatures of different points on the surface are different. The quantum nonthermal radiation characteristics of a black hole near the event horizon is also discussed by studying the Hamilton-Jacobi equation in curved spacetime and the maximum overlap of the positive and negative energy levels near the event horizon is given. There is a dimensional problem in the standard tortoise coordinate and the present results may be more reasonable. 相似文献
13.
Using the null geodesic method, Hawking radiation from the horizon of a Schwarzschild black hole is calculated. The thermodynamics can be built successfully on the horizon where the apparent horizon and event horizon are coincident with each other. When a relativistic perturbation is given to the horizon, the first law of thermodynamics can also be constructed at a new supersurface near the horizon successfully. The expressions of the characteristic position and temperature are consistent with the previous result while the thermodynamics was built on the event horizon in a Vaidya black hole. Therefore, the thermodynamics of a dynamical black hole should be constructed on the apparent horizon exactly, and the event horizon thermodynamics is just one of the perturbations near the apparent horizon. 相似文献
14.
The Hawking radiation of Dirac particles on the event horizon of a nonuniformly rectilinearly accelerating black hole is studied in this paper. First, we construct the symmetrized null tetrad from which the spin coefficients and Dirac equation are derived. Next, by proposing generalized tortoise coordinate transformation, the decoupling problem of the Dirac equation with nonzero rest mass is solved. Finally, by analytic continuation, the Hawking thermal spectrum formula of Dirac particle for nonuniformly rectilinearly accelerating black hole is obtained. 相似文献
15.
Treating macro-black hole as quantum states, and using Brown–York's quasi-local gravitational energy definition and Heisenberg uncertainty principle, the GHS black hole's quantum horizon is constructed. The Hawking temperature is computed naturally, and the entropy can also be figured out without introducing the cutoff factor h. The Φ-field mode number is predicted too. The result is consistent with that of the Schwarzschild and R-N black hole. 相似文献
16.
Kenji Muneyuki Nobuyoshi Ohta 《The European Physical Journal C - Particles and Fields》2012,72(1):1858
We study Hawking radiation in a new class of black hole solutions in Einstein–Gauss–Bonnet theory. The black hole has been
argued to have vanishing mass and entropy, but finite Hawking temperature. To check if it really emits radiation, we analyze
Hawking radiation using the original method of quantization of a scalar field in the black hole background and with the quantum
tunneling method, and confirm that it emits radiation at the Hawking temperature. A general formula is derived for the Hawking
temperature and backreaction in the tunneling approach. Physical implications of these results are discussed. 相似文献
17.
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.
关键词:
缓变动态黑洞
Hawking辐射
黑洞熵 相似文献
18.
We apply the non-equilibrium fluctuation theorems developed in the statistical physics to the thermodynamics of black hole horizons. In particular, we consider a scalar field in a black hole background. The system of the scalar field behaves stochastically due to the absorption of energy into the black hole and emission of the Hawking radiation from the black hole horizon. We derive the stochastic equations, i.e. Langevin and Fokker-Planck equations for a scalar field in a black hole background in the ?→0 limit with the Hawking temperature ?κ/2π fixed. We consider two cases, one confined in a box with a black hole at the center and the other in contact with a heat bath with temperature different from the Hawking temperature. In the first case, the system eventually becomes equilibrium with the Hawking temperature while in the second case there is an energy flow between the black hole and the heat bath. Applying the fluctuation theorems to these cases, we derive the generalized second law of black hole thermodynamics. In the present paper, we treat the black hole as a constant background geometry.Since the paper is also aimed to connect two different areas of physics, non-equilibrium physics and black holes physics, we include pedagogical reviews on the stochastic approaches to the non-equilibrium fluctuation theorems and some basics of black holes physics. 相似文献
19.
As realistic objects in the Universe, the black holes are surrounded by complex environment. By taking the effect of thermal environment into account, we investigate the evaporation process and the time evolutions (page curves) of the entanglement entropies of Hawking radiation of various types of black holes. It is found that the black holes with the thermal environments evaporate slower than those without the environments due to the environmental contribution of the energy flux in addition to Hawking radiation. For Schwarzschild black hole and Reissner-Nordström black hole in flat spaces, when the initial temperature of the black hole is higher than the environment temperature, the black holes evaporate completely and the Hawking radiation is eventually purified. For Schwarzschild-AdS black hole, it will evaporate completely and the Hawking radiation is purified when the environment temperature is lower than the critical temperature. Otherwise, it will reach an equilibrium state with the environment and the radiation is maximally entangled with the black hole. Our results indicate that the final state of the black hole is determined by the environmental temperature and the temporal evolution and the speed of the information purification process characterized by the page curve of the Hawking radiation is also influenced by the thermal environment significantly. 相似文献
20.
G. E. Volovik 《JETP Letters》2016,104(9):645-648
The type-II Weyl and type-II Dirac fermions may emerge behind the event horizon of black holes. Correspondingly, the black hole can be simulated by creation of the region with overtilted Weyl or Dirac cones. The filling of the electronic states inside the “black hole” is accompanied by Hawking radiation. The Hawking temperature in the Weyl semimetals can reach the room temperature, if the black hole region is sufficiently small, and thus the effective gravity at the horizon is large. 相似文献