Kiselev黑洞的热力学性质和物质吸积特性
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摘要
本文考虑带有黑洞视界和宇宙视界的Kiselev时空.研究以黑洞视界和宇宙视界为边界的系统的热力学性质.统一地给出了两个系统的热力学第一定律;在黑洞视界半径远小于宇宙视界半径的情况下,近似地计算了通过宇宙视界和黑洞视界的热能.然后,探讨Kiselev时空的物质吸积特性.在吸积能量密度正比于背景能量密度的条件下给出黑洞的吸积率,讨论了黑洞吸积率与暗能量态方程参数的关系.
Kiselev black hole possesses the two horizons, i.e. the inner horizon and outer horizon. In some cases, the so-called outer horizon of black hole is actually a cosmic horizon. In this paper, Kiselev space-time with black hole horizon and cosmic horizon is considered. The radius of black hole horizon and the radius of cosmic horizon are approximately obtained to be r_B≈2 M[1 +(2 M/λ)-~((3 w)q+1))] and r_C≈λ+2 M/3 w_q+1 with M <<λ and w_q a parameter. The energy density of the Kiselev spacetime near the cosmic horizon is approximately proportional to w_q, so the energy densities with some different w_q have the same order of magnitude in the range-1
Kiselev black hole possesses the two horizons, i.e. the inner horizon and outer horizon. In some cases, the so-called outer horizon of black hole is actually a cosmic horizon. In this paper, Kiselev space-time with black hole horizon and cosmic horizon is considered. The radius of black hole horizon and the radius of cosmic horizon are approximately obtained to be r_B≈2 M[1 +(2 M/λ)-~((3 w)q+1))] and r_C≈λ+2 M/3 w_q+1 with M <<λ and w_q a parameter. The energy density of the Kiselev spacetime near the cosmic horizon is approximately proportional to w_q, so the energy densities with some different w_q have the same order of magnitude in the range-1
引文
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[4] Kiselev V V 2003 Class. Quant. Grav. 20 1187
[5] Majeed B, Jamil M, Pradhan P 2015 Adv. High Energy Phys.2015 124910
[6] Azreg-Ainou M, Rodrigues M E 2013 J. High Energy Phys.2013 146
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[12] Jawad A, Shahzad M U 2016 Eur. Phys. J. C 76 123
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[14] Babichev E, Dokuchaev V, Eroshenko Y 2004 Phys. Rev.Lett. 93 021102
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[17] Gao C, Chen X, Faraoni V, Shen Y G 2008 Phys. Rev. D 78024008
[18] Babichev E, Chernov S, Dokuchaev V, Eroshenko Y 2008Phys. Rev. D 78 104027
[19] Kumar R, Ghosh S G 2017 Eur. Phys. J. C 77 577
[20] Paik B, Gangopadhyay S 2018 Int. J. Mod. Phys. A 331850084
[21] Ahmed A K, Camci U, Jamil M 2016 Class. Quantum Grav.33 215012
[22] Sharif M, Iftikhar S 2016 Eur. Phys. J. C 76 147
[23] Jiao L, Yang R J 2017 J. Cosmol. Astropart. Phys. 9 023
[24] Jiao L, Yang R J 2017 Eur. Phys. J. C77 356
[25] Sahoo P K, Mahanta K L, Goit D, Sihna A K, Xulu S S, Das U R, Prasad A, Prasad R 2015 Chin. Phys. Lett. 32 020402
[2] Perlmutter S, Aldering G, Goldhaber G, et al. 1999Astrophys. J. 517 565
[3] Garnavich P M, Kirshner R P, Challis P, et al. 1998Astrophys. J. 493 L53
[4] Kiselev V V 2003 Class. Quant. Grav. 20 1187
[5] Majeed B, Jamil M, Pradhan P 2015 Adv. High Energy Phys.2015 124910
[6] Azreg-Ainou M, Rodrigues M E 2013 J. High Energy Phys.2013 146
[7] Bondi H, Hoyle F 1944 Mon. Not. Roy. Astron. Soc. 104 273
[8] Bondi H 1952 Mon. Not. Roy. Astron. Soc. 112 195
[9] Michel F C 1972 Astrophys. Space Sci. 15 153
[10] Begelman M 1978 Astron. Astrophys. 70 583
[11] Malec E 1999 Phys. Rev. D 60 104043
[12] Jawad A, Shahzad M U 2016 Eur. Phys. J. C 76 123
[13] Karkowski J, Malec E 2013 Phys. Rev. D 87 044007
[14] Babichev E, Dokuchaev V, Eroshenko Y 2004 Phys. Rev.Lett. 93 021102
[15] Babichev E, Dokuchaev V, Eroshenko Y 2005 J. Exp. Theor.Phys. 100 528
[16] Jamil M, Rashid M A, Qadir A 2008 Eur. Phys. J. C 58 325
[17] Gao C, Chen X, Faraoni V, Shen Y G 2008 Phys. Rev. D 78024008
[18] Babichev E, Chernov S, Dokuchaev V, Eroshenko Y 2008Phys. Rev. D 78 104027
[19] Kumar R, Ghosh S G 2017 Eur. Phys. J. C 77 577
[20] Paik B, Gangopadhyay S 2018 Int. J. Mod. Phys. A 331850084
[21] Ahmed A K, Camci U, Jamil M 2016 Class. Quantum Grav.33 215012
[22] Sharif M, Iftikhar S 2016 Eur. Phys. J. C 76 147
[23] Jiao L, Yang R J 2017 J. Cosmol. Astropart. Phys. 9 023
[24] Jiao L, Yang R J 2017 Eur. Phys. J. C77 356
[25] Sahoo P K, Mahanta K L, Goit D, Sihna A K, Xulu S S, Das U R, Prasad A, Prasad R 2015 Chin. Phys. Lett. 32 020402