黑洞熵與黑洞似正規(guī)模的研究
發(fā)布時間：2018-11-12 20:41
【摘要】： 黑洞熵和黑洞似正規(guī)模一直是黑洞物理研究中的兩個前沿熱門課題。在黑洞熵的研究中,其統(tǒng)計力學(xué)起源問題尤為重要,但卻一直是困擾理論物理學(xué)者的一大難題。因此,對黑洞熵統(tǒng)計起源問題的深入研究將對黑洞物理學(xué)乃至量子引力理論的發(fā)展起到重要的推動作用。另外,黑洞似正規(guī)模與外場的初始擾動無關(guān),而是由黑洞自身的參數(shù)決定。這一特點說明,黑洞作為一種天體,它有自己的“特征聲音”,而似正規(guī)模正是這種“聲音”的物理表述。當不久的將來引力波被探測到時,黑洞似正規(guī)�？赡軙蔀楹诙创嬖诘闹苯幼C據(jù)。 本論文包括如下五部分內(nèi)容： 在第一章中,首先簡單回顧了黑洞及其熱力學(xué)性質(zhì),接著,介紹了黑洞熵和黑洞似正規(guī)模的定義、研究方法以及意義。 在第二章中,首先應(yīng)用薄膜模型方法計算了帶電dilaton-axion黑洞在漸進平直和漸進非平直兩種時空背景下的熵。通過計算視界面附近一薄層內(nèi)量子場的熵來得到黑洞熵。計算過程中,雖然克服了原始磚墻模型中的部分不完美之處,但仍然需要人為的引入截斷因子來消除視界面上的奇異。當把廣義測不準原理引入到了薄膜模型中計算黑洞熵時,在無需引入任何截斷因子的情形下,視界面附近量子場的發(fā)散問題就能夠被消除,并且小質(zhì)量近似問題也能夠很好的得以解決。然后,利用留數(shù)定理對黑洞熵的積分表達式進行計算,便能夠得到與視界面積成正比的黑洞熵。 在第三章中,采用三階WKB近似方法,分別計算了靜態(tài)球?qū)ΨQquintessence物質(zhì)包圍的整體單極子黑洞的有質(zhì)量標量場和無質(zhì)量Dirac場的低頻似正規(guī)模,并且詳細討論了似正規(guī)模頻率與各種參數(shù)因子之間的變化關(guān)系。 在第四章中,計算了在變形Horava-Lifshitz引力中的靜態(tài)球?qū)ΨQ黑洞的無質(zhì)量Dirac場的低頻似正規(guī)模,并且討論了Horava-Lifshitz參數(shù)因子對似正規(guī)模的影響。 最后是本論文的結(jié)論部分。
[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.
【學(xué)位授予單位】：大連理工大學(xué)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2010
【分類號】：P145.8
本文編號：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.
【學(xué)位授予單位】：大連理工大學(xué)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2010
【分類號】：P145.8
【參考文獻】
相關(guān)博士學(xué)位論文 前2條
1 常加峰;半經(jīng)典近似與黑洞低頻似正規(guī)模[D];中國科學(xué)院研究生院（上海天文臺）;2006年
2 陳松柏;黑洞時空中的似正規(guī)模和冪率拖尾[D];湖南師范大學(xué);2006年
，本文編號：2328162
本文鏈接：http://sikaile.net/kejilunwen/tianwen/2328162.html
教材專著
