带有整体单极的Reissner-Nordstrom-AdS黑洞在扩展相空间中的霍金辐射

韩亦文; 胡成; 洪云

doi:10.7498/aps.73.20231277

摘要

本文研究了带有整体单极的Reissner-Nordstrom-AdS黑洞在扩展相空间中出射粒子的量子隧穿辐射过程. 其中, 将宇宙学参数视为动态变量而不同于之前研究工作中将其视为常数而忽略其贡献. 具体地, 在计算出射粒子隧穿率时将宇宙学参数引入计算并将其解释为热力学压强. 计算结果表明, 出射粒子的隧穿率与粒子出射前后黑洞的贝肯斯坦-霍金熵差成正比, 辐射谱偏离了纯热谱, 该结果与将宇宙学参数视为常数的情况完全相同. 这意味着在扩展相空间中可以得到粒子的隧穿概率, 并且隧穿过程不依赖于热力学状参量, 这一工作自然地进一步将霍金辐射推广到了带有整体单极Reissner-Nordstrom-AdS黑洞扩展相空间中. 结果表明, 整体单极子尽管影响粒子的动力学行为和热力学量, 但并不影响熵变和隧穿率.

关键词:

Abstract

In recent years, thermodynamics and phase transitions of black holes in extended phase space have been extensively studied. The results show that the original first law of thermodynamics needs revising and new phase transitions will appear. However, so far, Hawking tunneling radiation has not been widely studied in the extended phase space. In particular, whether the tunneling radiation probability changes at this time is still uncertain. This work focuses on this topic, that is, to calculate the specific value of the tunneling probability in the extended phase space and ascertains whether the results obtained in the normal phase space are consistent with those in the extended phase space. The methods used herein are described below. Taking Reissner-Nordstrom-AdS black holes with global monopole for example, the cosmological parameters are regarded as dynamic variables, which is different from previous treatment methods that regard them as constants and ignore their contributions to the tunneling probability. In particular, cosmological parameters are introduced and regarded as thermodynamic pressure when the tunneling probability is calculated, and their contribution to the tunneling probability is considered. In the work the tunneling process of mass particles is mainly studied. The outgoing particles are viewed as spherical de Broglie waves, and then the relative phase velocity and group velocity are calculated. The geodesic equation is obtained according to the relationship between the two velocities, and the tunneling probability is calculated from the geodesic equation. It is concluded that the results show that the tunneling probability of the ingoing particles is proportional to the difference in the Bekenstein-Hawking entropy of the black hole before and after the particles tunnel, and the radiation spectrum deviates from the pure thermal spectrum, which is exactly the same as the case that the cosmological parameters are treated as constants. This means that the tunneling probability of particles can be obtained in the extended phase space, and the tunneling process does not depend on thermodynamic parameters. In addition, it is found that although the global monopole affects the dynamical behavior and thermodynamic quantity of the particle, it does not affect the entropy change or tunneling rate. In other words, the conclusion that the tunneling probability in extended phase space is exactly the same as that in normal phase space does not depend on the space-time topology.

Keywords:

作者及机构信息

1.
重庆工商大学物理系, 重庆　400067

2.
成都东软学院基础教学学院, 成都　611844

通信作者: 韩亦文, hanyw1965@163.com

基金项目: 重庆科技局基础研究项目(批准号: CSTB2023NSCQ-MSX0594)资助的课题.

Authors and contacts

1.
Department of Physics, Chongqing Technology and Business University, Chongqing 400067, China

2.
College of Basic Teaching, Chengdu Neuss of University, Chengdu 611844, China

Corresponding author: Han Yi-Wen, hanyw1965@163.com

Funds: Project supported by the Basic Research of Science and Technology Committee of Chongqing, China (Grant No. CSTB2023NSCQ-MSX0594).

文章全文 : translate this paragraph

参考文献

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施引文献

[1]	Akiyama K, Alberdi A, Alef W, et al. 2019 Astrophys. J. Lett. 875 L1 Google Scholar
[2]	Hawking S W 1974 Nature 248 30 Google Scholar
[3]	Hawking S W 1975 Commun. Math. Phys. 43 199 Google Scholar
[4]	Christodoulou D 1970 Phys. Rev. Lett. 25 1596 Google Scholar
[5]	BardeenJ M 1970 Nature 226 64 Google Scholar
[6]	Bekenstein J D 1973 Phys. Rev. D 7 2333 Google Scholar
[7]	Damour T, Ruffini R 1976 Phys. Rev. D 14 332 Google Scholar
[8]	Gibbons G W, Hawking S W 1977 Phys. Rev. D 15 2752 Google Scholar
[9]	York J W 1986 Phys. Rev. D 33 2091 Google Scholar
[10]	Whiting B F, York J W 1988 Phys. Rev. Lett. 61 1336 Google Scholar
[11]	Punsly B 1992 Phys. Rev. D 46 1288 Google Scholar
[12]	Srinivasan K, Padmanabhan T 1999 Phys. Rev. D 60 024007 Google Scholar
[13]	Robinson S P, Wilczek F 2005 Phys. Rev. Lett. 95 011303 Google Scholar
[14]	Han Y W, Zhang J Y 2010 Phys. Lett. B 692 74 Google Scholar
[15]	Han Y W, Chen G 2012 Phys. Lett. B 714 127 Google Scholar
[16]	ParikhM K, Wilczek F 2000 Phys. Rev. Lett. 85 5042 Google Scholar
[17]	Hemming S, Keski-Vakkuri E 2001 Phys. Rev. D 64 044006 Google Scholar
[18]	Vagenas E C 2002 Phys. Lett. B 533 302 Google Scholar
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[20]	Setare M R, Vagenas E C 2004 Phys. Lett. B 584 127 Google Scholar
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[23]	Medved A J M, Vagenas E C 2005 Mod. Phys. Lett. A 20 2449 Google Scholar
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[25]	韩亦文 2005 54 5018 Google Scholar Han Y W 2005 Acta Phys. Sin. 54 5018 Google Scholar
[26]	Han Y W 2005 Chin. Phys. Lett. 22 2769 Google Scholar
[27]	张靖仪, 赵峥 2006 55 3796 Google Scholar Zhang J Y, Zhao Z 2006 Acta Phys. Sin. 55 3796 Google Scholar
[28]	Liu W 2006 Phys. Lett. B 634 541 Google Scholar
[29]	Han Y W 2007 Chin. Phys. 16 0923 Google Scholar
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[40]	Caceres E, Nguyen P H, Pedraza J F 2015 JHEP 2015 184 Google Scholar
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[42]	Caldarelli M M, Cognola G, Klemm D 2000 Class. Quantum Grav. 17 399 Google Scholar
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[45]	Kubizňák D, Mann R B 2012 JHEP 2012 33 Google Scholar
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[47]	Cvetič M, Gibbons G W, Kubizňák D 2011 Phys. Rev. D 84 024037 Google Scholar
[48]	Altamirano N, Kubizňák D, Mann R B 2013 Phys. Rev. D 88 101502 Google Scholar
[49]	Dolan B P, Kostouki A, Kubizňák D 2014 Class. Quant. Grav. 31 242001 Google Scholar
[50]	Hennigar R A, Mann R B, Tjoa E 2017 Phys. Rev. Lett. 118 021301 Google Scholar
[51]	Wei S W, Liu Y X, Mann R B 2019 Phys. Rev. Lett. 123 071103 Google Scholar
[52]	Zeng X X, Han Y W, Che D Y 2019 Chin. Phys. C 43 105104 Google Scholar
[53]	Han Y W, Zeng X X, Hong Y 2019 Eur. Phys. J. C 79 252 Google Scholar
[54]	Ren Z X, Zeng X X, Han Y W, Hu C 2023 Nucl. Phys. B 990 116153 Google Scholar
[55]	Barriola M, Vilenkin A 1989 Phys. Rev. Lett. 63 341 Google Scholar
[56]	Yu H W 1994 Nucl. Phys. B 430 427 Google Scholar
[57]	He A, Tao J, Wang P, Xue Y, Zhang L 2022 Eur. Phys. J. C 82 683 Google Scholar
[58]	Chen S, Wang L, Ding C, et al. 2010 Nucl. Phys. B 836 222 Google Scholar
[59]	曾晓雄, 胡馨匀, 韩亦文, 刘显明 2015 中国科学: 物理学力学天文学 45 080401 Google Scholar Zeng X X, Hu X Y, Han Y W, Liu X M 2015 Sci. China-Phys. Mech. Astron. 45 080401 Google Scholar
[60]	周亮, 张靖仪 2010 59 4380 Google Scholar Zhou L, Zhang J Y 2010 Acta Phys. Sin. 59 4380 Google Scholar
[61]	Gao C J, Sen Y G 2002 Chin. Phys. Lett. 19 477 Google Scholar
[62]	Painlevé P 1921 Comptes Rendus Academie des Sciences (Serie Non Specifiee) 173 677
[63]	Gullstrand A 1922 Arkiv. Mat. Astron. Fys. 16 15

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