發(fā)布時間：2018-04-01 07:09

  本文選題：黑洞　切入點：熱力學　出處：《湖南師范大學》2016年碩士論文

【摘要】：黑洞熱力學性質作為黑洞的最重要的特性之一,一直廣泛的被學者們所研究。Bekenstein [1]首先提出黑洞的視界具有熱力學性質。隨后,和熱力學四定律相類似的黑洞熱力學四定律被提出。同時Hawking [2]指出,黑洞并不是完全黑的,它能以一種理想的黑體譜輻射粒子。1974年,Bekenst-ein[3]指出,黑洞的面積譜是均勻分布的,并且給出了面積譜的表達式An=nγlp2。從此黑洞的譜學也成為了一個很熱門的研究領域而被很多學者所研究。Hod[7]重新給出了面積譜的表達式并指出面積譜是與似正模的性質有關的,接著Dreyer [8]運用關于黑洞的似正模譜的經典引力理論又對面積譜的表達式進行了修正,Kunstatter [9]提出了絕熱不變量,并且指出這個絕熱不變量也擁有均勻分布的譜。Maggiore [10]對黑洞似正規(guī)模型的譜作出了解釋。Zeng [11]等人利用與擾亂黑洞的振動頻率相關聯(lián)的行波的運動周期,成功的把黑洞的視界面進行了量子化。在以上研究的基礎上,黑洞熱力學和譜學被國際國內的很多學者廣泛的關注,進行了大量的相關研究。另外,隨著宇宙的加速膨脹被提出,很多學者為了解釋這種現(xiàn)象提出假設,我們的宇宙中存在著一個外來的標量場,它提供了大量的負壓并組成了我們宇宙的百分之七十,我們稱之為暗能量。quintessence是被廣泛討論的一種暗能量模型,Kiselev [43]得到了被quintessence包圍的黑洞的靜態(tài)球對稱精確解,隨后Songhai Chen, Nijo Varghese和V C Kuriskose [44,45]分別在他們的文章里討論了被quintessence包圍的黑洞的似正模。Reissner-Nordstrom (R-N)黑洞是帶荷電的靜態(tài)球對稱黑洞,本文主要討論了quintessence場影響下的R-N黑洞的熱力學與譜學性質。本文通過繪制熱力學量隨quintessence參量的變化圖研究quintessence對其熱力學性質的影響,并且我們運用絕熱不變量滿足Born-Sommerfeld量子化規(guī)則運算得出了面積譜,并通過繪圖得出雖然面積譜與黑洞參量相關,但是面積分布是均勻的并且與熱力學參量無關。
[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 緯 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.
【學位授予單位】：湖南師范大學
【學位級別】：碩士
【學位授予年份】：2016
【分類號】：P145.8
，

本文編號：1694479