旋转压缩视界Kaluza-Klein黑洞时空中的强引力透镜

发布时间：2018-01-16 21:00

  本文关键词：旋转压缩视界Kaluza-Klein黑洞时空中的强引力透镜　出处：《湖南师范大学》2015年硕士论文　论文类型：学位论文

  更多相关文章： 黑洞 引力透镜 额外维 Kaluza-Klein 旋转

【摘要】：广义相对论指出物质及其运动将导致时空的弯曲从而使得经过其附近的光线发生偏转,这就是引力透镜效应。引力透镜效应被广泛应用于暗物质分布的探测,宇宙常数的限定,遥远暗淡星体的观测等诸多领域,也可用于检验和鉴别广义相对论和高维弦理论等各种引力理论。强引力透镜效应是指光线经过强引力场发生大角度偏转的现象。当光线经过光球半径附近时,它可以绕透镜天体若干圈再出射形成相对论像；在理论上黑洞的两侧可产生无穷多个相对论像；通过观测这些像的角位置与相对亮度,可以推断中心天体的结构和时空参数。本文将对旋转压缩视界Kaluza-Klein (KK)黑洞时空中的强引力透镜现象进行研究。在第一章,我们对引力透镜的基本原理,分类,和应用进行简单介绍；并介绍计算偏转角,放大率及成像位置的基本公式。在第二章,我们将介绍V.Bozza研究球对称静态黑洞时空中强引力透镜问题所提出的偏转角公式。V.Bozza的工作表明,当光线的径向坐标驻点x0不断趋近光球半径xm时,光线偏转角呈对数增长,最终趋于发散。利用强场近似方法,V.Bozza建立起了度规参数与强引力透镜的各观测量之间的联系,为通过对强引力透镜现象的观测来推断透镜天体的时空结构提供了理论依据。在第三章,我们应用V.Bozza的方法,研究了旋转压缩视界Kaluza-Klein黑洞时空中的强引力透镜效应,并与四维Kerr黑洞时空以及Godel压缩视界KK黑洞时空中的强引力透镜效应做了对比,总结这些不同类型的旋转参数对黑洞强引力透镜的影响。我们发现：(1)在旋转压缩视界KK黑洞时空中,光球半径脑,强引力透镜偏转角公式中的系数a,b,φ方向的偏转角a(θ),以及相应的观测量与光线在赤道面上的绕行方向无关。Godel压缩视界KK黑洞时空中的强引力透镜效应也具有相似的性质。这是压缩视界KK黑洞时空强引力透镜效应与Kerr旋转黑洞时空中强引力透镜效应一个截然不同的性质。(2)旋转压缩视界KK黑洞时空中,当旋转参数b固定时,光球半径ρps及相应的像的角位置θ∞随额外维尺度ρ0的增加先减小后增加。而在Godel压缩视界KK黑洞中,当旋转参数j较小时,光球半径ρps及相应的像的角位置θ∞随额外维尺度ρ0增加单调递增；当旋转参数j较大时,则这些量随之递减。(3)在极限压缩情形ρ0=0下,旋转压缩视界KK黑洞时空中的强引力透镜偏转角公式系数a随旋转参数单调增加,而在Godel压缩视界KK黑洞时空中,它则是一个不随旋转参数变化的常数。最后,我们对旋转压缩视界KK黑洞时空的强引力透镜效应的研究进行了总结和对将来的研究做了一些展望。
[Abstract]:The general theory of relativity points out that matter and its motion will cause the curvature of space and time to deflect the light passing through its vicinity, which is called gravitational lensing effect, which is widely used in the detection of dark matter distribution. The limitation of cosmic constant, the observation of distant dim stars and so on. It can also be used to test and distinguish various gravitational theories such as general relativity theory and high dimensional string theory. Strong gravitational lensing effect refers to the phenomenon of large angle deflection of light through strong gravitational field. It can circle the lens object several times and then shoot out to form a relativistic image. Theoretically, an infinite number of relativistic images can be produced on both sides of a black hole. By observing the angular position and relative brightness of these images. The structure and space-time parameters of the central celestial body can be inferred. In this paper, the phenomenon of strong gravitational lensing in the spacetime of the Kaluza-Klein KK black hole at the event horizon of rotation compression is studied. The basic principle, classification and application of gravitational lensing are briefly introduced. The basic formulas for calculating deflection angle, magnification and imaging position are also introduced in chapter 2. We will introduce V. Bozza's work on the deflection angle formula of V. Bozza for studying the problem of strong gravitational lensing in space-time of spherically symmetric static black hole. When the radial coordinates of the ray stationary point x0 keep approaching the radius of the light sphere x m, the deflection angle of the light increases logarithm and eventually tends to diverge. The strong field approximation method is used. V.Bozza has established a relationship between the metric parameters and the observations of a strong gravitational lens. This paper provides a theoretical basis for inferring the space-time structure of lens objects by observing the phenomena of strong gravitational lensing. In Chapter 3, we apply V. Bozza's method. The strong gravitational lensing effect in the spacetime of Kaluza-Klein black hole at the event horizon of rotation compression is studied. The results are compared with the strong gravitational lensing effect in four-dimensional Kerr black hole spacetime and Godel squeezed KK black hole spacetime. In this paper, we summarize the effect of these kinds of rotation parameters on the strong gravitational lensing of black hole. We find that the coefficient a in the formula of deflection angle of strong gravitational lens in the space and time of KK black hole at the event horizon of rotation compression is the radius of light sphere brain and the deflection angle of strong gravitational lens. The deflection angle a (胃) in the direction of b, 蠁. The strong gravitational lensing effect in the spacetime of the KK black hole at the event horizon of Godel squeezing has similar properties. This is the strong space-time property of the squeezed horizon KK black hole. The gravitational lensing effect is a very different property from the strong gravitational lensing effect in the spacetime of Kerr rotating black hole. 2) the space time of the KK black hole at the event horizon of rotation compression. When the rotation parameter b is fixed, the radius 蟻 PS and the angular position 胃 鈭，

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