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球对称动态黑洞Dirac场的统计熵 被引量:38
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作者 孟庆苗 苏九清 李传安 《物理学报》 SCIE EI CAS CSCD 北大核心 2003年第7期1822-1826,共5页
利用改进的brick wall模型 ,计算最一般球对称动态黑洞Dirac场的统计熵 .结果表明 ,任一时刻黑洞熵都与黑洞事件视界面积成正比 .特别是给出了动比例系数的计算公式 ,通过计算动比例系数 。
关键词 球对称 动态黑洞 DIRAC场 统计熵 动比例系数 事件视界 BRICK-WALL模型
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一般球对称带电蒸发黑洞的温度 被引量:32
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作者 宋太平 姚国政 《物理学报》 SCIE EI CAS CSCD 北大核心 2002年第5期1144-1148,共5页
从视界附近的Klein Gordon方程出发 ,准确地定出了一般球对称带电蒸发黑洞的Hawking温度和辐射谱 ,同时计算出事件视界方程 .所得结果与用零曲面方程得到的结果一致 .
关键词 一般球对称带电蒸发黑洞 温度 视界 辐射谱 热力学
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黑洞的普朗克绝对熵公式 被引量:31
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作者 李传安 《物理学报》 SCIE EI CAS CSCD 北大核心 2001年第5期986-989,共4页
利用黑洞热力学第一定律和第三定律分别导出黑洞的普朗克绝对熵公式 ,该公式表明黑洞熵与黑洞视界的全面积成正比 .
关键词 黑洞 普朗克绝对熵 热力学第一定律 热力学第三定律 黑洞熵 黑洞视界 经典热力学熵
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Vaidya黑洞周围时空中标量粒子的能量 被引量:26
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作者 孟庆苗 《徐州师范大学学报(自然科学版)》 CAS 2004年第2期40-42,共3页
利用弯曲时空中标量粒子运动的Hamilton Jacobi方程,研究Vaidya黑洞周围时空中标量粒子的能量.粒子的能量不仅与粒子的质量有关,还与黑洞的时空结构及视界的变化有关.
关键词 VAIDYA黑洞 时空中标量粒子 能量 HAMILTON-JACOBI方程 乌龟变换
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Vaidya-Bonner黑洞的熵 被引量:21
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作者 宋太平 侯晨霞 史旺林 《物理学报》 SCIE EI CAS CSCD 北大核心 2002年第6期1398-1402,共5页
从零曲面方程出发 ,得到了Vaidya Bonner黑洞的视界 ;利用Klein Gordon方程和薄膜Brick Wall模型 ,并采用WKB近似方法 ,求出了Vaidya Bonner黑洞的熵 ,所得的熵正好与该黑洞的视界面积成正比 .
关键词 Vaidya-Bonner黑洞 薄膜Brick-Wall模型 视界 零曲面方程
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视界邻域的几何与黑洞熵 被引量:14
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作者 李翔 赵峥 《北京师范大学学报(自然科学版)》 CAS CSCD 北大核心 2000年第1期69-74,共6页
视界邻域的时空具有类似Rindler度规的几何结构 ,从这个背景下的场方程出发 ,利用brick wall方法分别计算了标量场和Dirac场的熵 ,很自然地得到熵与面积成正比的结果 .这一结果适用于一大类黑洞 .还讨论了极端黑洞熵 ,指出拓扑熵只有经... 视界邻域的时空具有类似Rindler度规的几何结构 ,从这个背景下的场方程出发 ,利用brick wall方法分别计算了标量场和Dirac场的熵 ,很自然地得到熵与面积成正比的结果 .这一结果适用于一大类黑洞 .还讨论了极端黑洞熵 ,指出拓扑熵只有经典意义而不是量子的观点 . 展开更多
关键词 Rindler度规 黑洞熵 几何结构 视界领域
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一般球对称带电蒸发黑洞的熵 被引量:13
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作者 宋太平 侯晨霞 黄金书 《物理学报》 SCIE EI CAS CSCD 北大核心 2002年第8期1901-1906,共6页
从一般球对称带电蒸发黑洞的时空线元和零曲面方程出发 ,得到了该黑洞的视界 ;利用Klein Gordon方程求得波数 ,进而采用Wenzel Kramers Brillouin近似方法和薄膜brick wall模型 ,求出了一般球对称带电蒸发黑洞的熵 。
关键词 KLEIN-GORDON方程 薄膜brick-wall模型 视界 球对称带电蒸发黑洞
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动态广义球对称含荷黑洞的量子熵 被引量:9
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作者 刘成周 《物理学报》 SCIE EI CAS CSCD 北大核心 2005年第5期1977-1981,共5页
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... 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 . 展开更多
关键词 广义不确定原理 黑洞熵 量子场 截断 二维膜模型
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Time-periodic solutions of the Einstein's field equations Ⅰ:general framework 被引量:5
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作者 KONG DeXing1 & LIU KeFeng2 1Department of Mathematics,Zhejiang University,Hangzhou 310027,China 2Department of Mathematics,University of California at Los Angeles,CA 90095,USA 《Science China Mathematics》 SCIE 2010年第5期176-193,共18页
In this paper,we develop a new algorithm to find the exact solutions of the Einstein's field equations.Time-periodic solutions are constructed by using the new algorithm.The singularities of the time-periodic solu... In this paper,we develop a new algorithm to find the exact solutions of the Einstein's field equations.Time-periodic solutions are constructed by using the new algorithm.The singularities of the time-periodic solutions are investigated and some new physical phenomena,such as degenerate event horizon and time-periodic event horizon,are found.The applications of these solutions in modern cosmology and general relativity are expected. 展开更多
关键词 Einstein’s field equations time-periodic solution RIEMANN CURVATURE TENSOR SINGULARITY event horizon
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The Solution of the Einstein’s Equations in the Vacuum Region Surrounding a Spherically Symmetric Mass Distribution
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作者 Carlo Maria Pace 《Journal of Modern Physics》 2024年第9期1353-1374,共22页
In this article, we address the solution of the Einstein’s equations in the vacuum region surrounding a spherically symmetric mass distribution. There are two different types of mathematical solutions, depending on t... In this article, we address the solution of the Einstein’s equations in the vacuum region surrounding a spherically symmetric mass distribution. There are two different types of mathematical solutions, depending on the value of a constant of integration. These two types of solutions are analysed from a physical point of view. The comparison with the linear theory limit is also considered. This leads to a new solution, different from the well known one. If one considers the observational data in the weak field limit this new solution is in agreement with the available data. While the traditional Schwarzschild solution is characterized by a horizon at r=2GM/c2, no horizon exists in this new solution. 展开更多
关键词 General Theory of Relativity Schwarzschild Solution event horizon Black Hole
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The Unified Field
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作者 Joseph H. (Cass) Forrington 《Journal of Modern Physics》 2024年第7期1010-1035,共26页
This is a Unified Field description based on the holographic Time Dilation Cosmology, TDC, model, which is an eternal continuum evolving forward in the forward direction of time, at the speed of light, c, at an invari... This is a Unified Field description based on the holographic Time Dilation Cosmology, TDC, model, which is an eternal continuum evolving forward in the forward direction of time, at the speed of light, c, at an invariant 1 s/s rate of time. This is the Fundamental Direction of Evolution, FDE. There is also an evolution down time dilation gradients, the Gravitational Direction of Evolution, GDE. These evolutions are gravity, which is the evolutionary force in time. Gravitational velocities are compensation for the difference in the rate of time, dRt, in a dilation field, and the dRtis equal to the compensatory velocity’s percentage of c, and is a measure of the force in time inducing the velocity. In applied force induced velocities, the dRt is a measure of the resistance in time to the induced velocity, which might be called “anti-gravity” or “negative gravity”. The two effects keep the continuum uniformly evolving forward at c. It is demonstrated that gravity is already a part of the electromagnetic field equations in way of the dRt element contained in the TDC velocity formula. Einstein’s energy formula is defined as a velocity formula and a modified version is used for charged elementary particle solutions. A time dilation-based derivation of the Lorentz force ties gravity directly to the electromagnetic field proving the unified field of gravity and the EMF. It is noted how we could possibly create gravity drives. This is followed by a discussion of black holes, proving supermassive objects, like massive black hole singularities, are impossible, and that black holes are massless Magnetospheric Eternally Collapsing Objects (MECOs) that are vortices in spacetime. . 展开更多
关键词 Unified Field GRAVITY Anti-Gravity Astrophysics Einstein General Relativity Special Relativity Galactic Rotation Velocities Time Dilation SPACETIME Space Time Spacetime Continuum Quantum Continuum MECO Black Hole event horizon Timelike Spacelike Lightlike
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The Correct Reissner-Nordstrøm, Kerr and Kerr-Newman Metrics
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作者 Carlo Maria Pace 《Journal of Modern Physics》 2024年第10期1502-1522,共21页
In a very recent article of mine I have corrected the traditional derivation of the Schwarzschild metric thus arriving to formulate a correct Schwarzschild metric different from the traditional Schwarzschild metric. I... In a very recent article of mine I have corrected the traditional derivation of the Schwarzschild metric thus arriving to formulate a correct Schwarzschild metric different from the traditional Schwarzschild metric. In this article, starting from this correct Schwarzschild metric, I also propose corrections to the other traditional Reissner-Nordstrøm, Kerr and Kerr-Newman metrics on the basis of the fact that these metrics should be equal to the correct Schwarzschild metric in the borderline case in which they reduce to the case described by this metric. In this way, we see that, like the correct Schwarzschild metric, also the correct Reissner-Nordstrøm, Kerr and Kerr-Newman metrics do not present any event horizon (and therefore do not present any black hole) unlike the traditional Reissner-Nordstrøm, Kerr and Kerr-Newman metrics. 展开更多
关键词 General Theory of Relativity SCHWARZSCHILD Reissner-Nordstrøm KERR Kerr-Newman Metric event horizon Black Hole
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Where Is Phase Velocity in Minkowski Space?
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作者 Antony J. Bourdillon 《Journal of Modern Physics》 2024年第10期1555-1566,共12页
In the special theory of relativity, massive particles can travel at neither the speed of light c nor faster. Meanwhile, since the photon was quantized, many have thought of it as a point particle. How pointed? The id... In the special theory of relativity, massive particles can travel at neither the speed of light c nor faster. Meanwhile, since the photon was quantized, many have thought of it as a point particle. How pointed? The idea could be a mathematical device or physical simplification. By contrast, the preceding notion of wave-group duality has two velocities: a group velocity vg and a phase velocity vp. In light vp = vg = c;but it follows from special relativity that, in massive particles, vp > c. The phase velocity is the product of the two best measured variables, and so their product constitutes internal motion that travels, verifiably, faster than light. How does vp then appear in Minkowski space? For light, the spatio-temporal Lorentz invariant metric is s2=c2t2−x2−y2−z2, the same in whatever frame it is viewed. The space is divided into 3 parts: firstly a cone, symmetric about the vertical axis ct > 0 that represents the world line of a stationary particle while the conical surface at s = 0 represents the locus for light rays that travel at the speed of light c. Since no real thing travels faster than the speed of light c, the surface is also a horizon for what can be seen by an observer starting from the origin at time t = 0. Secondly, an inverted cone represents, equivalently, time past. Thirdly, outside the cones, inaccessible space. The phase velocity vp, group velocity vg and speed of light are all equal in free space, vp = vg = c, constant. By contrast, for particles, where causality is due to particle interactions having rest mass mo > 0, we have to employ the Klein-Gordon equation with s2=c2t2−x2−y2−z2+mo2c2. Now special relativity requires a complication: vp.vg = c2 where vg c and therefore vp > c. In the volume outside the cones, causality due to light interactions cannot extend beyond the cones. However, since vp > c and even vp >> c when wavelength λ is long, extreme phase velocities are then limited in their causal effects by the particle uncertainty σ, i.e. to vgt ± σ/ω, where ω is 展开更多
关键词 event horizon Scattering Range Wave Packet Phase Velocity Group Velocity Dispersion Dynamics Quantum Physics
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Time-periodic solutions of the Einstein's field equations II:geometric singularities 被引量:3
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作者 KONG DeXing1,LIU KeFeng2,& SHEN Ming3 1Department of Mathematics,Zhejiang University,Hangzhou 310027,China 2Department of Mathematics,University of California at Los Angeles,CA 90095,USA 3Center of Mathematical Sciences,Zhejiang University,Hangzhou 310027,China 《Science China Mathematics》 SCIE 2010年第6期1507-1520,共14页
In this paper,we construct several kinds of new time-periodic solutions of the vacuum Einstein's field equations whose Riemann curvature tensors vanish,keep finite or take the infinity at some points in these spac... In this paper,we construct several kinds of new time-periodic solutions of the vacuum Einstein's field equations whose Riemann curvature tensors vanish,keep finite or take the infinity at some points in these space-times,respectively.The singularities of these new time-periodic solutions are investigated and some new physical phenomena are discovered. 展开更多
关键词 Einstein’s field equations time-periodic solution RIEMANN curvature TENSOR SINGULARITY event horizon
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Tunnelling effect from a Vaidya-de Sitter black hole 被引量:5
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作者 任军 赵峥 《Chinese Physics B》 SCIE EI CAS CSCD 2006年第2期292-295,共4页
In this paper, we extend Parikh' recent work to the Vaidya-de Sitter black hole which is non-stationary. We view Hawking radiation as a tunnelling process across the event horizon and calculate the tunnelling probabi... In this paper, we extend Parikh' recent work to the Vaidya-de Sitter black hole which is non-stationary. We view Hawking radiation as a tunnelling process across the event horizon and calculate the tunnelling probability when the particle crosses the event horizon. From the tunnelling probability we also find a leading correction to the semiclassical emission rate. 展开更多
关键词 tunnelling effect Bondi mass event horizon
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基于四次方程的三角解研究非球对称动态黑洞的“类视界面” 被引量:6
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作者 成谢锋 陶冶薇 +1 位作者 李传安 苏九清 《工程数学学报》 CSCD 北大核心 2002年第3期39-44,共6页
给出了具有实用价值的四次方程的三角解正根公式 ,并以匀加速直线运动的Kerr黑洞为例 ,成功的研究了非球对称动态黑洞的“类视界面”。
关键词 四次方程 三角解 非球对称动态黑洞 类视界面
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黑洞熵公式的简单推导 被引量:5
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作者 李翔 赵峥 《北京师范大学学报(自然科学版)》 CAS CSCD 北大核心 2000年第2期193-194,共2页
Black hole is treated as 2 D membrane. Starting from the usual state equation of thermal radiation, the black hole entropy is technically computed, and the result that is proportional to the area of horizon is briefly... Black hole is treated as 2 D membrane. Starting from the usual state equation of thermal radiation, the black hole entropy is technically computed, and the result that is proportional to the area of horizon is briefly obtained. 展开更多
关键词 黑洞熵 视界 内禀性质 熵密度 辐射体系
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Identifying the Spatial Structure of Black Hole and Tropical Cyclone Based on a Theoretical Analysis of Orthogonal Interaction
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作者 Weihong Qian 《Journal of Modern Physics》 CAS 2023年第6期933-952,共20页
Black holes are recognized by Newton’s gravitational theory and Einstein’s general relativity, but there is still a lack of understanding the spatial structure of events, especially the nature of event horizon. In t... Black holes are recognized by Newton’s gravitational theory and Einstein’s general relativity, but there is still a lack of understanding the spatial structure of events, especially the nature of event horizon. In this paper, a theoretical analysis is used to compare the structures of tropical cyclone in the atmosphere and black hole in the astronomy so that five results are: 1) Both of them share the similar spatial structure, with tropical cyclone and black hole having the outflow cloud shield and the horizon sphere in the central part, respectively, while four spiral material bands exist in the rotating plane around them;2) In theoretically, the energy density formed by the orthogonal interaction of the four spiral material bands is as times as the total kinetic energy of the head-on interaction;3) This region of high energy density can lead to the conversion from mass to energy and the creation of new physical states of matter, which is a black hole event;4) The outer horizon of a black hole is the outermost interface of events, or the orthogonal interaction interface of particles;5) High-speed plasma jets extended at the poles of the black hole are directly associated with the shear stress of orthogonal interaction. 展开更多
关键词 Black Hole event horizon Tropical Cyclone Spatial Structure Orthographic Interaction
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P-Tree Structures and Event Horizon: Efficient Event-Set Implementations 被引量:1
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作者 Katerina Asdre Stavros D. Nikolopoulos 《Journal of Computer Science & Technology》 SCIE EI CSCD 2006年第1期19-26,共8页
This paper describes efficient data structures, namely the Indexed P-tree, Block P-tree, and Indexed-Block P-tree (or/P-tree, BP-tree, and IBP-tree, respectively, for short), for maintaining future events in a gener... This paper describes efficient data structures, namely the Indexed P-tree, Block P-tree, and Indexed-Block P-tree (or/P-tree, BP-tree, and IBP-tree, respectively, for short), for maintaining future events in a general purpose discrete event simulation system, and studies the performance of their event set algorithms under the event horizon principle. For comparison reasons, some well-known event set algorithms have been selected and studied, that is, the Dynamic-heap and the P-tree algorithms. To gain insight into the performance of the proposed event set algorithms and allow comparisons with the other selected algorithms, they are tested under a wide variety of conditions in an experimental way. The time needed for the execution of the Hold operation is taken as the measure for estimating the average time complexity of the algorithms. The experimental results show that the BP-tree algorithm and the IBP-tree algorithm behave very well with the event set of all the sizes and their performance is almost independent of the stochastic distributions. 展开更多
关键词 discrete-event simulation event set algorithms hold model event horizon data structures HEAP P-TREE P-tree structures
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Hawking radiation from a Vaidya black hole by Hamilton-Jacobi method 被引量:2
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作者 丁乾 刘文彪 《Frontiers of physics》 SCIE CSCD 2011年第1期106-108,共3页
Using the Hamilton Jacobi method, Hawking radiation from the apparent horizon of a dynamical Vaidya black hole is calculated. The black hole thermodynamics can be built successfully on the apparent horizon. If a relat... Using the Hamilton Jacobi method, Hawking radiation from the apparent horizon of a dynamical Vaidya black hole is calculated. The black hole thermodynamics can be built successfully on the apparent horizon. If a relativistic perturbation is given to the apparent horizon, a similar calculation can also lead to a purely thermal spectrum, which corresponds to a modified temperature from the former. The first law of thermodynamics can also be constructed successfully at a new supersurface which has a small deviation from the apparent horizon. When the event horizon is thought as such a deviation from the apparent horizon, the expressions of the characteristic position and temperature are consistent with the previous result that asserts that thermodynamics should be built on the event horizon. It is concluded that the thermodynamics should be constructed on the apparent horizon exactly while the event horizon thermodynamics is just one of the perturbations near the apparent horizon. 展开更多
关键词 Vaidya black hole Hawking radiation apparent horizon event horizon THERMODYNAMICS
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