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Thermodynamics of extremal rotating thin shells in an extremal BTZ spacetime and the extremal black hole entropy

机译:极值旋转薄壳在极值BTZ时空和极值黑洞熵中的热力学

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摘要

In a (2 + 1)-dimensional spacetime with a negative cosmological constant, the thermodynamics and the entropy of an extremal rotating thin shell, i.e., an extremal rotating ring, are investigated. The outer and inner regions with respect to the shell are taken to be the Ba?ados-Teitelbom-Zanelli (BTZ) spacetime and the vacuum ground state anti-de Sitter spacetime, respectively. By applying the first law of thermodynamics to the extremal thin shell, one shows that the entropy of the shell is an arbitrary well-behaved function of the gravitational area A_+ alone, S = S(A_+).When the thin shell approaches its own gravitational radius r_+ and turns into an extremal rotating BTZ black hole, it is found that the entropy of the spacetime remains such a function of A_+, both when the local temperature of the shell at the gravitational radius is zero and nonzero. It is thus vindicated by this analysis that extremal black holes, here extremal BTZ black holes, have different properties from the corresponding nonextremal black holes, which have a definite entropy, the Bekenstein-Hawking entropy S(A_+)= A_+/4G, where G is the gravitational constant. It is argued that for extremal black holes, in particular for extremal BTZ black holes, one should set 0 ≤ S(A_+) ≤ A_+/4G; i.e., the extremal black hole entropy has values in between zero and the maximum Bekenstein-Hawking entropy A_+/4G. Thus, rather than having just two entropies for extremal black holes, as previous results have debated, namely, 0 and A_+/4G, it is shown here that extremal black holes, in particular extremal BTZ black holes, may have a continuous range of entropies, limited by precisely those two entropies. Surely, the entropy that a particular extremal black hole picks must depend on past processes, notably on how it was formed. A remarkable relation between the third law of thermodynamics and the impossibility for a massive body to reach the velocity of light is also found. In addition, in the procedure, it b
机译:在(2 + 1) - 具有负宇宙常数的二维时期,研究了热力学和极端旋转薄壳的熵,即极端旋转环。相对于壳体的外部和内部区域被认为是BA?Ados-Teitelbom-Zanelli(BTZ)时空和真空接地状态抗DE STETTER SPACETIME。通过将第一热力学定律应用于极端薄壳,一个人表示壳体的熵是重力区域A_ +的任意良好的函数,S = S(A _ +)。当薄壳接近其时拥有引力半径R_ +并变成极端旋转的BTZ黑洞,发现时空的熵仍然是A_ +的功能,当壳体在引力半径的壳体的局部温度为零和非零时都是这样的。因此,通过这种分析来证明,极端黑洞,这里极值的BTZ黑洞,具有不同的非惊人的黑洞的性质,具有明确的熵,Bekenstein-hapking熵s(a _ +)= a _ + / 4g,其中g是引力常数。有人认为,对于极端黑洞,特别是对于极值BTZ黑洞,一个应该设置0≤S(A_ +)≤A_ + / 4g;即,极值黑洞熵在零和最大Bekenstein-hapking熵之间具有_ + / 4g之间的值。因此,而不是仅仅具有用于极值黑洞的两个熵,即以前的结果已经争论,即0和_ + / 4g,这里示出了极端黑洞,特别是极值BTZ黑洞,可以具有连续的范围熵,限制了这两个熵。当然,特定极值黑洞选择的熵必须依赖于过去的过程,特别是关于它的形成方式。还发现了热力学的第三定律与巨大身体达到光速之间的不可能性之间的显着关系。另外,在手术中,它是b

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  • 来源
    《Physical review, D》 |2017年第1期|共14页
  • 作者单位

    Centro Multidisciplinar de Astrofísica-CENTRA Departamento de Física Instituto Superior Técnico-IST Universidade de Lisboa-UL Avenida Rovisco Pais 1 1049-001 Lisboa Portugal;

    Centro Multidisciplinar de Astrofísica-CENTRA Departamento de Física Instituto Superior Técnico-IST Universidade de Lisboa-UL Avenida Rovisco Pais 1 1049-001 Lisboa Portugal;

    Department of Physics and Technology Kharkov V. N. Karazin National University 4 Svoboda Square Kharkov 61022 Ukraine and Institute of Mathematics and Mechanics Kazan Federal University 18 Kremlyovskaya St. Kazan 420008 Russia;

  • 收录信息
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 粒子物理学;场论;
  • 关键词

    Thermodynamics; extremal; rotating;

    机译:热力学;极值;旋转;

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