The total quantum statistical entropy of Reissner-Nordstrom (RN) black holes is evaluated. The spacetime of the black holes is divided into three regions-region 1, (r > ro);region 2, (ro > r > ri);andregion 3...The total quantum statistical entropy of Reissner-Nordstrom (RN) black holes is evaluated. The spacetime of the black holes is divided into three regions-region 1, (r > ro);region 2, (ro > r > ri);andregion 3, (ri > r > 0)-where ro is the radius of the outer event horizon, and ri is the radius of the inner event horizon. The total quantum statistical entropy of RN black holes is S = S1 + S2 + Ss, where Si (i = 1, 2, 3) is the entropy, contributed by region Si (i = 1, 2, 3). The detailed calculation shows that S2 ≈ 0. S1 = (π^(2)/45)[kbAo/∈^(2)β^(3)], S3 = -(r2/45)[kbAi/∈^(2)β^(3)], where Ao and Ai are, respectively, the area of the outer and inner event horizons. Thus, as ri approaches ro, in the extreme case the total quantum statistical entropy of RN black holes approaches zero.展开更多
The free energy and entropy of a general spherically symmetry black hole are calculated by quantum statistic method with brick wall model Two different kinds of approximation are used to calculate the number of states...The free energy and entropy of a general spherically symmetry black hole are calculated by quantum statistic method with brick wall model Two different kinds of approximation are used to calculate the number of states in transverse spatial space. The final results are approximately equal except a rational numerical constant. The formulas of free energy and entropy, evaluated by each one of the two different kinds of approximation, are the same except some numerical constants. The free energy and entropy are dependent on the spacetime dimensionsD. When D = 4, they reduce to the usual well known results.展开更多
Absorbing charged rotating(ACR)metric in de Sitter space and related energy-momentum tensor are derived.The ACR metric is very simple in advanced time coordinates.The ACR metric involves 8 independent parameters which...Absorbing charged rotating(ACR)metric in de Sitter space and related energy-momentum tensor are derived.The ACR metric is very simple in advanced time coordinates.The ACR metric involves 8 independent parameters which are divided into two c the mass M,charge Q,angular momentum per unit mass a,and cosmological constant A;(2)■M/■v,■^(2)M/■v^(2),■q/■V,and ■^(2)Q/■v^(2).The non-stationary part of the energy-momentum tensor is positive definite everywhere.展开更多
Metric of accelerating,radiating Kerr-Newman de Sitter black holes is derived in this letter.The metric involves(7+10)independent parameters.The volume density of space-time,and the electromagnetic potential in accele...Metric of accelerating,radiating Kerr-Newman de Sitter black holes is derived in this letter.The metric involves(7+10)independent parameters.The volume density of space-time,and the electromagnetic potential in accelerating,radiating cases are the same as in nonaccelerating,nonradiating cases.The space-time related to acceleration is not asymptotic Minkowski flat.So the energy momentum tensor is not positive definite.展开更多
As is known,the two-dimensional(2D)gravitational theory is a very good toy model for studying the four-dimensional gravitational theory.Now in this paper,it is shown that the vacuum fluctuation in 2D gravity can creat...As is known,the two-dimensional(2D)gravitational theory is a very good toy model for studying the four-dimensional gravitational theory.Now in this paper,it is shown that the vacuum fluctuation in 2D gravity can create a foam-like structure of space-time,which is constructed from wormhole.展开更多
The Kerr-NUT-de sitter metric in quasi-Boyer-Lindquest coordinate is derived by using the step-by-step extension method.The extension may be realized in several different paths.For example,one of these paths may be ch...The Kerr-NUT-de sitter metric in quasi-Boyer-Lindquest coordinate is derived by using the step-by-step extension method.The extension may be realized in several different paths.For example,one of these paths may be chosen as from Schwarzschild-NUT metric to Schwarzschild-NUT-de Sitter metric and from Schwarzschild-NUT-de Sitter metric to Kerr-NUT-de Sitter metric.展开更多
文摘The total quantum statistical entropy of Reissner-Nordstrom (RN) black holes is evaluated. The spacetime of the black holes is divided into three regions-region 1, (r > ro);region 2, (ro > r > ri);andregion 3, (ri > r > 0)-where ro is the radius of the outer event horizon, and ri is the radius of the inner event horizon. The total quantum statistical entropy of RN black holes is S = S1 + S2 + Ss, where Si (i = 1, 2, 3) is the entropy, contributed by region Si (i = 1, 2, 3). The detailed calculation shows that S2 ≈ 0. S1 = (π^(2)/45)[kbAo/∈^(2)β^(3)], S3 = -(r2/45)[kbAi/∈^(2)β^(3)], where Ao and Ai are, respectively, the area of the outer and inner event horizons. Thus, as ri approaches ro, in the extreme case the total quantum statistical entropy of RN black holes approaches zero.
文摘The free energy and entropy of a general spherically symmetry black hole are calculated by quantum statistic method with brick wall model Two different kinds of approximation are used to calculate the number of states in transverse spatial space. The final results are approximately equal except a rational numerical constant. The formulas of free energy and entropy, evaluated by each one of the two different kinds of approximation, are the same except some numerical constants. The free energy and entropy are dependent on the spacetime dimensionsD. When D = 4, they reduce to the usual well known results.
文摘Absorbing charged rotating(ACR)metric in de Sitter space and related energy-momentum tensor are derived.The ACR metric is very simple in advanced time coordinates.The ACR metric involves 8 independent parameters which are divided into two c the mass M,charge Q,angular momentum per unit mass a,and cosmological constant A;(2)■M/■v,■^(2)M/■v^(2),■q/■V,and ■^(2)Q/■v^(2).The non-stationary part of the energy-momentum tensor is positive definite everywhere.
文摘Metric of accelerating,radiating Kerr-Newman de Sitter black holes is derived in this letter.The metric involves(7+10)independent parameters.The volume density of space-time,and the electromagnetic potential in accelerating,radiating cases are the same as in nonaccelerating,nonradiating cases.The space-time related to acceleration is not asymptotic Minkowski flat.So the energy momentum tensor is not positive definite.
基金Supported by the National Natural Science Foundation of China under Grant No.19473005。
文摘As is known,the two-dimensional(2D)gravitational theory is a very good toy model for studying the four-dimensional gravitational theory.Now in this paper,it is shown that the vacuum fluctuation in 2D gravity can create a foam-like structure of space-time,which is constructed from wormhole.
基金Supported in part by the National Natural Science Foundation of China.
文摘The Kerr-NUT-de sitter metric in quasi-Boyer-Lindquest coordinate is derived by using the step-by-step extension method.The extension may be realized in several different paths.For example,one of these paths may be chosen as from Schwarzschild-NUT metric to Schwarzschild-NUT-de Sitter metric and from Schwarzschild-NUT-de Sitter metric to Kerr-NUT-de Sitter metric.
