精质场影响下的荷电黑洞的热力学与谱学

发布时间：2018-04-01 07:09

  本文选题：黑洞　切入点：热力学　出处：《湖南师范大学》2016年硕士论文

【摘要】：黑洞热力学性质作为黑洞的最重要的特性之一,一直广泛的被学者们所研究。Bekenstein [1]首先提出黑洞的视界具有热力学性质。随后,和热力学四定律相类似的黑洞热力学四定律被提出。同时Hawking [2]指出,黑洞并不是完全黑的,它能以一种理想的黑体谱辐射粒子。1974年,Bekenst-ein[3]指出,黑洞的面积谱是均匀分布的,并且给出了面积谱的表达式An=nγlp2。从此黑洞的谱学也成为了一个很热门的研究领域而被很多学者所研究。Hod[7]重新给出了面积谱的表达式并指出面积谱是与似正模的性质有关的,接着Dreyer [8]运用关于黑洞的似正模谱的经典引力理论又对面积谱的表达式进行了修正,Kunstatter [9]提出了绝热不变量,并且指出这个绝热不变量也拥有均匀分布的谱。Maggiore [10]对黑洞似正规模型的谱作出了解释。Zeng [11]等人利用与扰乱黑洞的振动频率相关联的行波的运动周期,成功的把黑洞的视界面进行了量子化。在以上研究的基础上,黑洞热力学和谱学被国际国内的很多学者广泛的关注,进行了大量的相关研究。另外,随着宇宙的加速膨胀被提出,很多学者为了解释这种现象提出假设,我们的宇宙中存在着一个外来的标量场,它提供了大量的负压并组成了我们宇宙的百分之七十,我们称之为暗能量。quintessence是被广泛讨论的一种暗能量模型,Kiselev [43]得到了被quintessence包围的黑洞的静态球对称精确解,随后Songhai Chen, Nijo Varghese和V C Kuriskose [44,45]分别在他们的文章里讨论了被quintessence包围的黑洞的似正模。Reissner-Nordstrom (R-N)黑洞是带荷电的静态球对称黑洞,本文主要讨论了quintessence场影响下的R-N黑洞的热力学与谱学性质。本文通过绘制热力学量随quintessence参量的变化图研究quintessence对其热力学性质的影响,并且我们运用绝热不变量满足Born-Sommerfeld量子化规则运算得出了面积谱,并通过绘图得出虽然面积谱与黑洞参量相关,但是面积分布是均匀的并且与热力学参量无关。
[Abstract]:As one of the most important properties of black holes, the thermodynamic properties of black holes have been extensively studied by many scholars. Bekenstein first proposed that the event horizon of black holes has thermodynamic properties. Four laws of black hole thermodynamics similar to the four laws of thermodynamics have been proposed. Meanwhile, Hawking [2] pointed out that black hole is not completely black, it can radiate particles with ideal blackbody spectrum. In 1974, Bekenst-ein [3] pointed out that the area spectrum of black hole is uniformly distributed. And the expression of area spectrum An=n 纬 LP 2 is given. Since then, the spectrum of black hole has also become a very popular research field, and has been studied by many scholars. Hod [7] regives the expression of area spectrum and points out that the area spectrum is related to the properties of quasi-positive modes. Then Dreyer [8] proposed an adiabatic invariant using the classical gravitational theory of the quasi-positive mode spectrum of a black hole and modified the expression of the area spectrum. It is also pointed out that the adiabatic invariant also has a uniformly distributed spectrum. Maggiore [10] explains the spectrum of the black hole quasi-normal model. Zeng [11] and others use the traveling wave period associated with disturbing the vibration frequency of the black hole. On the basis of the above research, black hole thermodynamics and spectroscopy have been widely concerned by many scholars at home and abroad, and a large number of related studies have been carried out. As the accelerating expansion of the universe was proposed, many scholars hypothesized that there was an external scalar field in our universe that provided a lot of negative pressure and made up 70% of our universe. We call it the dark energy. Quintessence is a widely discussed dark energy model. [43] the exact solution of the static spherical symmetry of a black hole surrounded by quintessence is obtained. Then Songhai Chen, Nijo Varghese and V C Kuriskose [44N45] discuss in their respective papers that the quasi-positive mode of the black hole surrounded by quintessence. Reissner-Nordstrom R-N) black hole is a charged static spherically symmetric black hole. In this paper, the thermodynamic and spectral properties of R-N black hole under the influence of quintessence field are mainly discussed. The influence of quintessence on the thermodynamic properties of R-N black hole is studied by drawing the diagram of the variation of thermodynamic quantities with quintessence parameters. The area spectrum is obtained by using adiabatic invariants to satisfy the Born-Sommerfeld quantization rule, and the area distribution is uniform and independent of thermodynamic parameters, although the area spectrum is related to the parameters of the black hole.
【学位授予单位】：湖南师范大学
【学位级别】：硕士
【学位授予年份】：2016
【分类号】：P145.8
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本文编号：1694479