广义不确定关系与整体单极黑洞Dirac场的熵

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.     

利用广义不确定关系计算Gibbons-Maeda黑洞的统计力学熵

利用广义不确定关系修正的态密度方程并采用WKB近似方法, 计算了Gibbons-Maeda黑洞时空中标量场的统计力学熵. 所得的统计力学熵与该黑洞的视界面积成正比, 与Brick-Wall方法所得的结果相同, 但不需要取任何截断就能避免Brick-Wall方法的发散问题. 关键词： 广义不确定关系 Gibbons-Maeda黑洞 态密度 统计力学熵     

静态球对称黑洞热力学与爱因斯坦场方程

建立在广义相对论基础上的黑洞理论与热力学定律之间有着深刻的内在联系.具体考虑球对称黑洞,研究表明通过史瓦西黑洞和Reissner-Nordstrom黑洞在其视界附近的爱因斯坦场方程可以直接得到对应的黑洞热力学第一定律.这揭示了爱因斯坦引力场方程与黑洞热力学的关系,表明了在广义相对论理论框架下黑洞热力学规律的必然性.     

利用广义不确定关系计算 Reissner-Nordström-de Sitter黑洞的统计力学熵

利用广义不确定关系修正的态密度方程并采用Wentzel-Kramers-Brillouin (WKB) 近似方法, 计算了Reissner-Nordström-de Sitter (RNdS) 黑洞时空中标量场的统计力学熵. 结果表明, 由这种方法得到的黑洞熵与它的内、外视界面积和宇宙视界面积之和成正比, 这与采用其他方法所得的结果一致, 从而揭示了黑洞熵与视界面积之间的内在联系, 也进一步表明了黑洞熵是视界面上量子态的熵, 是一种量子效应.     

利用广义不确定关系计算Reissner-Nordstrm-de Sitter黑洞的统计力学熵

利用广义不确定关系修正的态密度方程并采用Wentzel-Kramers-Brillouin(WKB)近似方法,计算了Reissner-Nordstrm-de Sitter(RNdS)黑洞时空中标量场的统计力学熵.结果表明,由这种方法得到的黑洞熵与它的内、外视界面积和宇宙视界面积之和成正比,这与采用其他方法所得的结果一致,从而揭示了黑洞熵与视界面积之间的内在联系,也进一步表明了黑洞熵是视界面上量子态的熵,是一种量子效应.     

广义Heisenberg不确定关系

对广义Ｈｅｉｓｅｎｂｅｒｇ不确定关系的多种形式，讨论了它们的由来、意义与适应范围；这将有助于对这些关系式的恰当理解和运用。     

辐射在黑洞视界附近的性质与热力学第二定律

考虑把一个装满某种内能为E,熵为S的物质的盒子缓慢地向黑洞降落,Bekenstein认为热力学第二定律成立的必要条件为S/E≤2πR(R为盒子的有效半径),而Unruh和Wald认为Hawking辐射的存在保证了广义热力学第二定律的成立,无需条件S/E≤2πR。我们指出:Hawking辐射和S/E≤2πR都无法保证热力学第二定律的成立。我们根据充分的理由提出:引力场会影响物质的态方程。当盒子中装的为辐射时,我们得出了辐射在视界附近时的态方程,它和平直时空的辐射的态方程很不一样。只要将方程中的某个参量加上适当的限制,即可保证热力学第二定律的成立。 关键词：     

动态广义球对称含荷黑洞的统计熵

利用改进了的brickwall膜模型,计算了动态广义球对称含荷黑洞的熵,研究结果表明,对于动态黑洞,将黑洞熵表示为与视界面积成正比时,则比例系数总与动态黑洞的视界速度有关 关键词： 广义球对称黑洞 黑洞熵 brick-wall膜模型 WKB近似     

动态广义球对称含荷黑洞的量子熵

计算了广义球对称含荷黑洞视界上标量场的量子态数和自由能，得到了黑洞熵与视界面积成 正比的结论，表明黑洞熵就是其视界上的量子态的熵．考虑广义不确定原理对黑洞熵的影响 ，采用二维膜模型，克服了brick-wall模型中的发散困难，计算中无须任何截断，且brick- wall模型中的小质量近似也可以避免．对视界外二维膜上的量子场的熵做了级数展开讨论， 得到了一些值得探讨的结论． 关键词： 广义不确定原理 黑洞熵 视界 截断     

广义测不准关系与三维BTZ黑洞熵

通过应用在量子引力中,由广义测不准关系得出的新的态密度方程,研究三维BTZ背景下黑洞的熵.当取广义测不准关系中引入的,具有Planck量级与空间维数有关的常数λ为特定值时,得到BTZ黑洞Bekenstein-Hawking 熵和修正项.由于利用新的态密度方程,在计算中不存在用brick-wall模型计算黑洞熵时出现的发散项和小质量近似.所得结论,从量子统计力学角度给出了黑洞Bekenstein-Hawking 熵的修正值,使人们对黑洞熵的修正值有更深入的认识. 关键词： 广义测不准关系 量子统计 BTZ黑洞熵     

Thermodynamics of the black holes under the extended generalized uncertainty principle with linear terms

In this paper, we employ the extended generalized uncertainty principle with linear terms (LEGUP) to investigate the thermodynamics properties of the Schwarzschild and Reissner–Nordström (RN) black holes. Firstly, by constructing the theoretical framework of LEGUP, the minimal temperature of the Schwarzschild black hole and the modified mass–temperature function for the black hole are calculated. Furthermore, the heat capacity function for the Schwarzschild black hole is obtained. After that, we compare LEGUP black hole thermodynamics with EGUP black hole and with the usual forms. Besides, the modification of black hole entropy is discussed, which involves a heuristic analysis of particles absorbed by the black hole. Finally, we derive the LEGUP-corrected temperature, heat capacity and entropy functions of the RN black hole.     

Subleading terms of thermodynamic quantities around static spherical black holes

The thermodynamic quantities for the gases of massless particles with spin s = 1 / 2, 1, 3 / 2, 2 around static spherical black holes are investigated by using the brick-wall method. The appearance of the spin-dependent subleading terms is demonstrated and the terms are shown to contain not only the linear and quadratic terms of the spins but also a zero-power term of the spins.     

静态球对称黑洞的热质点模型及辐射功率

利用静态球对称黑洞的热质点模型,研究了黑洞的热辐射规律,得到了当η取固有厚度时,对所有Schwarzschild黑洞,其辐射功率都相同,其视界处的辐射能通量与黑洞的质量的平方成反比,而距黑洞遥远的观察者所接收到的辐射能通量与观测者到黑洞的距离的平方成反比; Reissner-Nordstrm黑洞视界处的辐射能通量和辐射功率不仅与黑洞的质量有关,还与黑洞的电荷有关,而距黑洞遥远的观察者所接收到的辐射能通量,当截断的固有厚度η、黑洞的质量m和电荷Q取定后与观测者到黑洞之间的距离的 关键词： 静态球对称黑洞 热质点模型 辐射功率 辐射能通量     

Information entropy for static spherically symmetric black holes

By using the new equation of state density derived from the generalized uncertainty relation, the number of the quantum states near event horizon is obtained, with which then the information entropy of static spherically symmetric black holes has been discussed. It is found that the divergent integral of quantum states near the event horizon can be naturally avoided if using the new equation of state density without introducing the ultraviolet cut-off. The information entropy of black holes can be obtained precisely by the residue theorem, which is shown to be proportional to the horizon area. The information entropy of black holes obtained agrees with the Bechenstein--Hawking entropy when the suitable cutoff factor is adopted.     

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.     

Comparison of thermodynamic behaviors of two regular-AdS black holes

Considering the negative cosmological constant of an anti-de Sitter (AdS) background as a positive thermodynamic pressure in the extended phase space, we investigate the P−υ critical behavior and of the cooling–heating phase transition of the regular Hayward-AdS (HAdS) black hole (BH), and compare the difference of some thermodynamic processes in both the HAdS BH and the Bardeen-AdS (BAdS) BH. We found that the phase transition of the BAdS BH tends to be more the van der Waals (vdW) phase transition. For the cooling–heating phase transition, we obtained the inversion curves of the HAdS BH are always higher than the BAdS BH under the same pressure and magnetic charge. We also compare the smallest existence mass, the zero-temperature remnant, and the critical magnetic charge for these two BHs. The results suggested that the inner horizon and the outer horizon of the Hayward BH are easier to merge, and the singularity is easier to expose.     

Kerr 时空黑洞熵和测不准关系

通过应用在量子引力中、由广义测不准关系得出的新的态密度方程,直接求解轴对称Kerr黑洞背景下Bose场和Fermi场的配分函数.然后,在黑洞视界附近计算黑洞背景下Bose场和Fermi场的熵.在所得结论中不存在用brick wall模型计算黑洞熵时出现的发散项,也不存在紫外因子.得到黑洞熵与视界面积成正比的结论.