黑洞熵与黑洞似正规模的研究
发布时间：2018-11-12 20:41
【摘要】： 黑洞熵和黑洞似正规模一直是黑洞物理研究中的两个前沿热门课题。在黑洞熵的研究中,其统计力学起源问题尤为重要,但却一直是困扰理论物理学者的一大难题。因此,对黑洞熵统计起源问题的深入研究将对黑洞物理学乃至量子引力理论的发展起到重要的推动作用。另外,黑洞似正规模与外场的初始扰动无关,而是由黑洞自身的参数决定。这一特点说明,黑洞作为一种天体,它有自己的“特征声音”,而似正规模正是这种“声音”的物理表述。当不久的将来引力波被探测到时,黑洞似正规模可能会成为黑洞存在的直接证据。 本论文包括如下五部分内容： 在第一章中,首先简单回顾了黑洞及其热力学性质,接着,介绍了黑洞熵和黑洞似正规模的定义、研究方法以及意义。 在第二章中,首先应用薄膜模型方法计算了带电dilaton-axion黑洞在渐进平直和渐进非平直两种时空背景下的熵。通过计算视界面附近一薄层内量子场的熵来得到黑洞熵。计算过程中,虽然克服了原始砖墙模型中的部分不完美之处,但仍然需要人为的引入截断因子来消除视界面上的奇异。当把广义测不准原理引入到了薄膜模型中计算黑洞熵时,在无需引入任何截断因子的情形下,视界面附近量子场的发散问题就能够被消除,并且小质量近似问题也能够很好的得以解决。然后,利用留数定理对黑洞熵的积分表达式进行计算,便能够得到与视界面积成正比的黑洞熵。 在第三章中,采用三阶WKB近似方法,分别计算了静态球对称quintessence物质包围的整体单极子黑洞的有质量标量场和无质量Dirac场的低频似正规模,并且详细讨论了似正规模频率与各种参数因子之间的变化关系。 在第四章中,计算了在变形Horava-Lifshitz引力中的静态球对称黑洞的无质量Dirac场的低频似正规模,并且讨论了Horava-Lifshitz参数因子对似正规模的影响。 最后是本论文的结论部分。
[Abstract]:Black hole entropy and black hole size are two hot topics in black hole physics. In the study of black hole entropy, the origin of its statistical mechanics is particularly important, but it has always been a difficult problem for theoretical physicists. Therefore, the further study on the origin of entropy statistics will play an important role in the development of black hole physics and even the theory of quantum gravity. In addition, the size of the black hole is not related to the initial disturbance of the field, but is determined by the parameters of the black hole itself. This characteristic shows that black hole as a celestial body has its own "characteristic sound", and the physical expression of this "sound" is likely to be positive scale. When gravitational waves are detected in the near future, the size of black holes may be a direct evidence of the existence of black holes. This paper includes five parts as follows: in the first chapter, we briefly review the black hole and its thermodynamic properties, and then introduce the definition, research method and significance of black hole entropy and black hole like normal scale. In the second chapter, the entropy of charged dilaton-axion black hole under the background of asymptotic flatness and asymptotically non-flatness is calculated by using the thin film model method. The entropy of black hole is obtained by calculating the entropy of quantum field in a thin layer near the apparent interface. In the process of calculation, although some imperfections in the original brick wall model are overcome, the truncation factor is still needed to eliminate the singularity in the visual interface. When the generalized uncertainty principle is introduced into the film model to calculate the entropy of black hole, the divergence problem of quantum field near the apparent interface can be eliminated without introducing any truncation factor. And the problem of small quality approximation can also be well solved. Then, by using residue theorem to calculate the integral expression of black hole entropy, we can get black hole entropy which is proportional to the area of event horizon. In chapter 3, by using the third-order WKB approximation method, the mass scalar field and the low-frequency quasi-positive scale of the massless Dirac field of the global monopole black hole surrounded by static spherically symmetric quintessence matter are calculated, respectively. The relationship between the frequency of quasi-positive scale and various parameter factors is discussed in detail. In chapter 4, the low-frequency quasi-positive scale of the massless Dirac field of a static spherically symmetric black hole in deformed Horava-Lifshitz gravity is calculated, and the influence of the Horava-Lifshitz parameter factor on the quasi-positive scale is discussed. The last part is the conclusion of this paper.
【学位授予单位】：大连理工大学
【学位级别】：博士
【学位授予年份】：2010
【分类号】：P145.8
本文编号：2328162
[Abstract]:Black hole entropy and black hole size are two hot topics in black hole physics. In the study of black hole entropy, the origin of its statistical mechanics is particularly important, but it has always been a difficult problem for theoretical physicists. Therefore, the further study on the origin of entropy statistics will play an important role in the development of black hole physics and even the theory of quantum gravity. In addition, the size of the black hole is not related to the initial disturbance of the field, but is determined by the parameters of the black hole itself. This characteristic shows that black hole as a celestial body has its own "characteristic sound", and the physical expression of this "sound" is likely to be positive scale. When gravitational waves are detected in the near future, the size of black holes may be a direct evidence of the existence of black holes. This paper includes five parts as follows: in the first chapter, we briefly review the black hole and its thermodynamic properties, and then introduce the definition, research method and significance of black hole entropy and black hole like normal scale. In the second chapter, the entropy of charged dilaton-axion black hole under the background of asymptotic flatness and asymptotically non-flatness is calculated by using the thin film model method. The entropy of black hole is obtained by calculating the entropy of quantum field in a thin layer near the apparent interface. In the process of calculation, although some imperfections in the original brick wall model are overcome, the truncation factor is still needed to eliminate the singularity in the visual interface. When the generalized uncertainty principle is introduced into the film model to calculate the entropy of black hole, the divergence problem of quantum field near the apparent interface can be eliminated without introducing any truncation factor. And the problem of small quality approximation can also be well solved. Then, by using residue theorem to calculate the integral expression of black hole entropy, we can get black hole entropy which is proportional to the area of event horizon. In chapter 3, by using the third-order WKB approximation method, the mass scalar field and the low-frequency quasi-positive scale of the massless Dirac field of the global monopole black hole surrounded by static spherically symmetric quintessence matter are calculated, respectively. The relationship between the frequency of quasi-positive scale and various parameter factors is discussed in detail. In chapter 4, the low-frequency quasi-positive scale of the massless Dirac field of a static spherically symmetric black hole in deformed Horava-Lifshitz gravity is calculated, and the influence of the Horava-Lifshitz parameter factor on the quasi-positive scale is discussed. The last part is the conclusion of this paper.
【学位授予单位】：大连理工大学
【学位级别】：博士
【学位授予年份】：2010
【分类号】：P145.8
【参考文献】
相关博士学位论文 前2条
1 常加峰;半经典近似与黑洞低频似正规模[D];中国科学院研究生院（上海天文台）;2006年
2 陈松柏;黑洞时空中的似正规模和幂率拖尾[D];湖南师范大学;2006年
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