1)Vaidya black holeVaidya黑洞
1.We have applied Hamilton-Jacobi method to study the Hawking radiation as tunneling from non-stationary Vaidya black hole.采用Ham ilton-Jacob i方法对动态Vaidya黑洞的Hawk ing隧穿辐射进行研究,结果表明该黑洞的辐射谱不是纯热谱,且出射粒子的隧穿率与Bekenste in-Hawk ing熵变有关。
2.Quantum correction to the entropy of a Vaidya black hole due to high spin fields of spin quantum number 2 is studied by improved brick-wall model.利用改进后的brick-wall模型研究自旋为2的引力场对动态Vaidya黑洞熵的量子修正,作者发现,在动态Vaidya黑洞中,自旋为2的引力场的量子熵仍与黑洞的视界面积成正比;当选择与标量场相同的截断因子时,其熵为标量场的2倍,为Dirac场的4/7倍,引力场,标量场和Dirac场对黑洞熵的总贡献为38Ah。
3.Using the WKB approximation, the scalar field entropy of the horizon of the Vaidya black hole is calculated directly.把广义不确定关系引入黑洞熵的计算 ,采用WKB近似方法 ,对Vaidya黑洞视界面上的标量场的熵进行了直接计算 ,得到了熵与视界面积成正比的结论 ;与brick wall模型不同的是 ,我们得到的结果是有限的 ,无需任何截断 。
2)Vaidya-Bonner black holeVaidya-Bonner黑洞
1.Contribution of high spin field to the entropy of Vaidya-Bonner black hole;高自旋场对Vaidya-Bonner黑洞熵的贡献
2.Fermions tunneling of the Vaidya-Bonner black holeVaidya-Bonner黑洞的费米子隧穿
英文短句/例句
1.Fermions tunneling of the Vaidya-Bonner black holeVaidya-Bonner黑洞的费米子隧穿
2.Tunnelling effect from a Vaidya-Bonner black hole and corresponding emission spectrum correctionVaidya-Bonner黑洞的隧穿效应及出射修正谱
3.The Laplace operator in Vaidya-Bonner space-time;Vaidya-Bonner空时中的Laplace算符
4.Statistical Entropy of Schwarzschild Black Hole.;Schwarzschild黑洞的统计熵
5.Such spinning black holes are known as Kerr Black Holes.这种旋转的黑洞被称为克尔黑洞。
6.there was a deep, dark hole.有个又深又黑的洞，
7.There is a dark cave at the foot of the mountain.在山脚下有一个黑山洞。
8.Tom is peering into a dark cave.汤姆正朝黑洞里窥视。
9.One goes out,Black as ovens, indeed!出了门就是一个黑洞。
10.Statistical Entropy of Keer-Taub-NUT Black Hole;Keer-Taub-NUT黑洞的统计熵
11.The Planck s Radiation Formula of The Dirac Fieldin Black Hole;黑洞辐射Dirac场的Plank’s公式
12.Entropy of Dilaton-Maxwell black hole;动态Dilaton-Maxwell黑洞的熵
13.Statistical Entropy of the Dirac Field of statics Pherically Summrtric Black Hole of The Electric Charge;Schwarzschild黑洞Dirac场的统计熵
14.Crowds disgorged from the theatre into the dark street.人流从戏院涌出, 进入了黑洞洞的街道.
15.If we get to know something about them, black holes will not be that frightful.如果我们认识了黑洞,黑洞就不那么可怕了.
16.Black Hole Entropy, Black Hole Information Paradox & Quantum Teleportation in Curved Space-time;黑洞熵，黑洞信息佯谬及弯曲时空中的量子通讯
17.I or=# cc0066> grope for the light switch in the dark room.我在黑洞洞的屋里摸索著寻找电灯开关。
18.I grume for the light switch in the dark room我在黑洞洞的屋里摸索著寻找电灯开关
相关短句/例句
Vaidya-Bonner black holeVaidya-Bonner黑洞
1.Contribution of high spin field to the entropy of Vaidya-Bonner black hole;高自旋场对Vaidya-Bonner黑洞熵的贡献
2.Fermions tunneling of the Vaidya-Bonner black holeVaidya-Bonner黑洞的费米子隧穿
3)Vaidya-Bonner-de Sitter black holeVaidya-Bonner-deSitter黑洞
4)Vaidya-Bonner-de Sitter black holeVaidya-Bonner-de Sitter黑洞
1.Quantum entropy of the neutrino and scalar fields in Vaidya-Bonner-de Sitter black hole;Vaidya-Bonner-de Sitter黑洞背景下中微子场和标量场的量子熵
5)black hole黑洞
1.Routing algorithm defense against black hole attacks in MANET based on mobile agent;MANET环境中抵御“黑洞”攻击的路由算法
2.The energy of scalar particles in a generalized spherical symmetric evaporating charged black hole;广义球对称带电蒸发黑洞周围时空中标量粒子的能量
3.Entropy of the scalar field in general accelerating non-stationary black holes with electric charge and magnetic charge;一般加速带电带磁的动态黑洞中标量场的熵
6)black holes黑洞
1.In this method,the adjustable matching threshold is used to greatly reduce the number of black holes,improving fuzzy matching for control parameters with the prescribed fuzzy similarity.该算法匹配阈值可变,采用调整匹配阈值的方法大幅降低黑洞数量;在满足一定模糊相似度的前提下,实现了带控制参数的模糊匹配,模糊程度可控。
2.Global solutions of advection dominated accretion- flows (ADAFs) around black holes are presented.对黑洞径移主导吸积流（ＡＤＡＦ）的整体解作了研究。
3.The damage to the constant speed of Hawking s radiation done by motion layer around black holes is expounded and it is the important reason for the latter to remain undetectable.本文论述了黑洞周围运动层对霍金辐射恒定速度的破坏，是后者至今仍无法探测到的重要原因。
延伸阅读
黑洞黑洞blackhole广义相对论所预言的一种天体。一个质量比太阳大8倍以上的恒星，一般经过超新星爆发留下超过二、三个太阳质量的核，将没有任何力能阻止它继续坍缩。当它的半径小于引力半径rg＝2GM／c2（G为万有引力常数，c为光速，M为天体的质量）时，没有任何物质或辐射能够逃逸出来，成为黑洞。黑洞的性质由三个参量来表征，即质量M、角动量J和电荷Q。当J＝Q＝0时，它是球对称的史瓦西黑洞；当Q＝0时，则为轴对称的克尔黑洞。黑洞的性质决定了探测黑洞的困难性。如果向黑洞下落的气体具有较大的角动量，则应绕着黑洞在轨道上旋转，形成一个气盘。气盘中相邻层之间因气体的粘滞性引起的摩擦产生了热能，理论计算表明，气盘应具有很高温度，在X射线波段产生辐射。另一方面，黑洞的质量应大于中子星的质量上限，能够精确确定质量的是双星系统。因此，最有希望找到黑洞的是大质量X射线双星，尤其是天鹅座X-1。这是一个X射线变源，它有一个光学对应体，从这个9等超巨星的光谱得到视向速度的周期性变化，暗示一个不可见伴星的存在。进一步算出它的质量大于4太阳质量，很可能是8太阳质量，大于中子星的上限2～3太阳质量；另一个有希望的黑洞候选者是大麦哲伦云X-3，它也是一个X射线双星，其中不可见天体的质量也是8太阳质量。
