共查询到20条相似文献,搜索用时 31 毫秒
1.
In this paper,vacuum C-metric when m=0 is derived from the metric of a Schwarzschild black hole if its mass and location approach to infinity in an appropriate way.Furthermore,by using coordinate transformation in which there is no acceleration,vacuum C-metric when m=0 is transformed to Rindler metric.The result shows that an infinitesimal neighborhood of the horizon of an infinite Schwarzschild black hole is a Rindler space-time,and the acceleration in the Rindler space-time can arise from the in finite Schwarzschild black hole. 相似文献
2.
Rotating maximal black holes in four-dimensional de Sitter space, for which the outer event horizon coincides with the cosmological horizon, have an infinite near-horizon region described by the rotating Nariai metric. We show that the asymptotic symmetry group at the spacelike future boundary of the near-horizon region contains a Virasoro algebra with a real, positive central charge. This is evidence that quantum gravity in a rotating Nariai background is dual to a two-dimensional Euclidean conformal field theory. These results are related to the Kerr/CFT correspondence for extremal black holes, but have two key differences: one of the black hole event horizons has been traded for the cosmological horizon, and the near-horizon geometry is a fiber over dS2 rather than AdS2. 相似文献
3.
B. S. Ramachandra K. R. Nayak C. V. Vishveshwara 《General Relativity and Gravitation》2003,35(11):1977-2005
The Vaidya-Einstein-Kerr (VEK) black hole which represents the spacetime of the Kerr black hole in a non-vacuum, asymptotically non-flat background is investigated. The energy-momentum tensor corresponding to this spacetime satisfies reasonable energy conditions. We study several properties of this black hole and compare and contrast them with those of the Kerr black hole. We investigate the effect of the background on the geometry of the event horizon by computing the equatorial and polar circumferences and determining the oblateness of the horizon. We find that the surface area of the VEK black hole gets nontrivially coupled to rotation in sharp contrast to the Kerr case. We show that the angular velocity of the VEK horizon goes up significantly as the background influence increases. By using the `equatorial tangential velocity' of the VEK horizon we classify the horizon and define the `limiting black hole' a generalization that contains the extreme Kerr black hole as a special case. Finally we investigate the Gaussian curvature and establish conditions for global embedding of the VEK black hole in Euclidean space. 相似文献
4.
5.
Michael Streubel 《General Relativity and Gravitation》1978,9(7):597-619
A simple local geometric condition is given that is sufficient to restrict the possible variety of exterior fields of all stationary axisymmetric black hole spaces to depend only on a finite number of parameters. It is discussed how this condition could be used to gain insight into the nature of the Carter-Robinson uniqueness theorem. Also a new coordinate system is constructed for all stationary axially symmetric space-times possessing a bifurcate Killing horizon. It covers a whole neighborhood of the horizons and of the bifurcation axis and possesses special geometric properties that are easy to visualize. The Kerr metric together with its spin coefficients and Weyl tensor components are described in the new coordinates. 相似文献
6.
Ji-Jian Jiang Chuan-An Li Xie-Feng Cheng 《International Journal of Theoretical Physics》2016,55(8):3746-3751
By constructing the four-dimensional phase space based on the observable physical quantity of Kerr black hole and gauge transformation, the Kerr black hole entropy in the phase space was obtained. Then considering the corresponding mechanical quantities as operators and making the operators quantized, entropy spectrum of Kerr black hole was obtained. Our results show that the Kerr black hole has the entropy spectrum with equal intervals, which is in agreement with the idea of Bekenstein. In the limit of large event horizon, the area of the adjacent event horizon of the black hole have equal intervals. The results are in consistent with the results based on the loop quantum gravity theory by Dreyer et al. 相似文献
7.
V.A. Belinski 《Physics letters. A》2012,376(3):207-215
It is shown here that there is no way for particle creation to occur by quantum tunneling through an infinitesimal neighborhood of the black hole horizon. This result is a trivial consequence of the regularity of the horizon, the equivalence principle and the general covariance of the relativistic theory of gravity. Moreover, we also confirm the less trivial statement that no particle creation by quantum tunneling through the black hole horizon is possible independent of the size of the presupposed tunneling domain. 相似文献
8.
P C Vaidya 《Pramana》1977,8(6):512-517
A metric satisfying Einstein’s equations is given which in the vicinity of the source reduces to the well-known Kerr metric
and which at large distances reduces to the Robertson-Walker metric of a homogeneous cosmological model. The radius of the
event horizon of the Kerr black hole in the cosmological background is found out. 相似文献
9.
Edward Anderson 《General Relativity and Gravitation》2013,45(12):2545-2551
A coordinate system that blockwise-simplifies the Kerr–Newman black hole’s thermodynamical state space Ruppeiner metric geometry is constructed, with discussion of the limiting cases corresponding to simpler black holes. It is deduced that one of the three conformal Killing vectors of the Reissner–Nordström and Kerr cases (whose thermodynamical state space metrics are 2 by 2 and conformally flat) survives generalization to the Kerr–Newman case’s 3 by 3 thermodynamical state space metric. 相似文献
10.
In this paper we calculate the center-of-mass energy of two colliding test particles near the rotating and non-rotating Horava–Lifshitz
black hole. For the case of a slowly rotating KS solution of Horava–Lifshitz black hole we compare our results with the case
of Kerr black holes. We confirm the limited value of the center-of-mass energy for static black holes and unlimited value
of the center-of-mass energy for rotating black holes. Numerically, we discuss temperature dependence of the center-of-mass
energy on the black hole horizon. We obtain the critical angular momentum of particles. In this limit the center-of-mass energy
of two colliding particles in the neighborhood of the rotating Horava–Lifshitz black hole could be arbitrarily high. We found
appropriate conditions where the critical angular momentum could have an orbit outside the horizon. Finally, we obtain the
center-of-mass energy corresponding to this circle orbit. 相似文献
11.
O. B. Zaslavskii 《General Relativity and Gravitation》2018,50(10):123
We consider the metric of a generic axially symmetric rotating stationary black hole. The general approach is developed that enables us to construct coordinate frame regular near the horizon. As explicit examples, the Kerr and Kerr–Newmann-(anti-)de Sitter metrics are considered. It is shown how the rotational versions of the Painlevé–Gullstrand and Doran coordinates appear in this scheme as particular cases. For the 2 + 1 version of the metric the direct generalization of the Lemaître coordinate system is obtained. It is shown that the possibility of introducing a regular frame is indirectly related to the constancy of a black hole angular velocity and the rate with which the metric coefficient responsible for the rotation of spacetime tends to it. 相似文献
12.
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
13.
S. W. Hawking 《Communications in Mathematical Physics》1972,25(2):152-166
It is assumed that the singularities which occur in gravitational collapse are not visible from outside but are hidden behind an event horizon. This means that one can still predict the future outside the event horizon. A black hole on a spacelike surface is defined to be a connected component of the region of the surface bounded by the event horizon. As time increase, black holes may merge together but can never bifurcate. A black hole would be expected to settle down to a stationary state. It is shown that a stationary black hole must have topologically spherical boundary and must be axisymmetric if it is rotating. These results together with those of Israel and Carter go most of the way towards establishing the conjecture that any stationary black hole is a Kerr solution. Using this conjecture and the result that the surface area of black holes can never decrease, one can place certain limits on the amount of energy that can be extracted from black holes. 相似文献
14.
We show that an extremal Kerr black hole, appropriately lifted to M theory, can be transformed to a Kaluza-Klein black hole in M theory, or a D0-D6 charged black hole in string theory. Since all the microstates of the latter have recently been identified, one can exactly reproduce the entropy of an extremal Kerr black hole. We also show that the topology of the event horizon is not well defined in M theory. 相似文献
15.
利用黑洞的绝热不变性,研究了引力彩虹时空中Kerr黑洞的熵谱和面积谱.首先,在引力彩虹时空背景下,计算了Kerr黑洞的绝热不变作用量,并将其与玻尔-索末菲量子化条件相结合,给出了黑洞的熵谱.得到的熵谱没有引力彩虹时空本身具有的粒子能量依赖性,且是与经典Kerr黑洞中原始贝肯斯坦熵谱相同的等间距熵谱.然后,根据黑洞热力学第一定律和黑洞熵谱,给出了与原始贝肯斯坦谱不同的面积谱.该面积谱是非等间距的,而且有对黑洞面积的依赖性,但不依赖于探测粒子的能量.面积谱表明,随着黑洞面积的减少,面积间隔逐步变小;当黑洞达到普朗克尺度时,面积量子可降为零.这表示黑洞面积不再减少,黑洞出现辐射剩余.而在忽略色散关系的修正效应或在大黑洞极限下,面积谱的修正项可以忽略,引力彩虹Kerr黑洞面积谱可以回归到原始贝肯斯坦谱.此外,对引力彩虹时空Kerr黑洞的熵进行了讨论,得到了带有面积倒数修正项的黑洞熵,分析了黑洞熵的量子修正与面积谱量子修正的一致性. 相似文献
16.
It is a well known analytic result in general relativity that the 2-dimensional area of the apparent horizon of a black hole
remains invariant regardless of the motion of the observer, and in fact is independent of the t = constant slice, which can be quite arbitrary in general relativity. Nonetheless the explicit computation of horizon area is often
substantially more difficult in some frames (complicated by the coordinate form of the metric), than in other frames. Here
we give an explicit demonstration for very restricted metric forms of (Schwarzschild and Kerr) vacuum black holes. In the
Kerr–Schild coordinate expression for these spacetimes they have an explicit Lorentz-invariant form. We consider boosted versions with the black hole moving through the coordinate system. Since these are stationary black hole spacetimes, the
apparent horizons are two dimensional cross sections of their event horizons, so we compute the areas of apparent horizons
in the boosted space with (boosted) t = constant, and obtain the same result as in the unboosted case. Note that while the invariance of area is generic, we deal only with
black holes in the Kerr–Schild form, and consider only one particularly simple change of slicing which amounts to a boost.
Even with these restrictions we find that the results illuminate the physics of the horizon as a null surface and provide
a useful pedagogical tool. As far as we can determine, this is the first explicit calculation of this type demonstrating the
area invariance of horizons. Further, these calculations are directly relevant to transformations that arise in computational
representation of moving black holes. We present an application of this result to initial data for boosted black holes. 相似文献
17.
This paper delineates the first steps in a systematic quantitative study of the spacetime fluctuations induced by quantum
fields in an evaporating black hole. We explain how the stochastic gravity formalism can be a useful tool for that purpose
within a low-energy effective field theory approach to quantum gravity. As an explicit example we apply it to the study of
the spherically-symmetric sector of metric perturbations around an evaporating black hole background geometry. For macroscopic
black holes we find that those fluctuations grow and eventually become important when considering sufficiently long periods
of time (of the order of the evaporation time), but well before the Planckian regime is reached. In addition, the assumption
of a simple correlation between the fluctuations of the energy flux crossing the horizon and far from it, which was made in
earlier work on spherically-symmetric induced fluctuations, is carefully analyzed and found to be invalid. Our analysis suggests
the existence of an infinite amplitude for the fluctuations of the horizon as a three-dimensional hypersurface. We emphasize
the need for understanding and designing operational ways of probing quantum metric fluctuations near the horizon and extracting
physically meaningful information.
Dedicated to Rafael Sorkin on the occasion of his 60th birthday. 相似文献
18.
In this paper, we consider charged accelerating AdS black holes with nonlinear electromagnetic source. The metric chosen by us is of a regular black hole, which shows regular nature at poles and a conical effect, which corresponds to a cosmic string. In such a space time construction of the Lagrangian for a charged particle is done. Cyclic coordinates as well as the corresponding symmetry generators, i.e., the Killing vectors are found. Conservation laws corresponding to the symmetries are counted. Euler-Lagrange equations are found. The orbit is mainly taken to be a circular one and effective potential is found. The minimum velocity obtained by a particle to escape from innermost stable circular orbit is found. The value of this escape velocity is plotted with respect to the radius of the event horizon of the central black hole for different parametric values. The nature of the escape velocity is studied when the central object is working with gravitational force and charge simultaneously. Effective potential and effective force are also plotted. The range of radius of event horizon for which the effective force turns to be positive is found out. A pathway of future studies of accretion disc around such black holes is made. 相似文献
19.
It is known that the entropy for a singular spacetime metric can be calculated in the framework of classical field theories by applying Noether's theorem to stationary solutions of Einstein's field equations, integrating a suitable form on a trapping surface for the singularity. When the Kerr solution is considered, two different horizons appear. The physical entropy for the system is well known to be related to the outer horizon. We investigate here which is the meaning of the entropy calculated (via first principle of black hole thermodynamics) on the inner horizon. We show that this entropy, which was earlier interpreted as a sort of "spin entropy" of the black hole, admits in fact an interpretation as a quantity associated to a conserved charge which is related to the rotational degrees of freedom of the system. 相似文献
20.
Zhao Zheng 《International Journal of Theoretical Physics》1999,38(5):1539-1548
The thermal character of the inner horizon ofthe Kerr black hole is studied. There is a quantumthermal effect, Hawking absorption, nearthe inner horizon. We give a new formulation of the Bekenstein-Smarr formula and redefine theentropy of the black hole. The redefined entropy must goto zero as the temperature of the black hole approachesabsolute zero. The entropy satisfies the Nernst theorem, so it can be regarded as the Planckabsolute entropy of the Kerr black hole. 相似文献