一类新的Stckelberg全息超导模型

彭严; 邓方安; 刘国华; 杨凯凡

doi:10.7498/aps.64.157401

摘要

本文研究了含Stckelberg机理的黑洞全息超导模型. 通过选取标量场新的高阶修正形式, 建立了新的Stckelberg黑洞全息超导模型. 通过研究模型参数对标量场凝聚的影响, 发现了当模型参数大于临界值时, 高阶修正可以引起一阶相变. 同时本文还考查了反作用对临界值的影响.

关键词:

AdS/CFT对应性 /
黑洞 /
全息超导

The AdS/CFT correspondence has provided us a useful approach to describe strongly interacting systems holographically through weakly coupled gravitational duals. One of the mostly studied gravity duals is the holographic superconductor, which is constructed by a scalar field coupled to a Maxwell field in an AdS black hole background. It is shown that when the Hawking temperature of a black hole drops below a critical value, the black hole becomes unstable and this instability in the (d+1) dimensional AdS black hole corresponds to a d-dimensional phase transition at the boundary, called holographic superconductor model. Generally speaking, the instability of the gravity systems belongs to the second-order phase transition. Lately, it was stated that the holographic superconductor with the spontaneous breaking of a global U(1) symmetry via the Stckelberg mechanism allows the first-order phase transition to occur. Some further studies are carried out by considering new forms of the Stckelberg mechanism. So it is very interesting to extend the discussion to other new forms of Stckelberg mechanism to explore the rich properties of holographic superconductors. By considering new higher correction terms of the scalar fields, we investigate a general class of holographic superconductors via Stckelberg mechanism in the background of four-dimensional AdS black hole. We obtain richer structures in the metal/superconductor phase transitions. We study the condensation of the scalar operator and find that when the model parameter is above a threshold value, this new model allows first-order phase transition to occur. We also examine the effects of the backreaction on the threshold model parameter and find that backreaction makes the first-order phase transitions easier to happen (or smaller threshold parameters above which the phase transition changes from second to first order). We may conclude that the model parameter coupled with the backreaction can determine the order of phase transitions.

Keywords:

作者及机构信息

1.
陕西理工学院, 数学与计算机科学学院, 汉中 723000

基金项目: 国家自然科学基金青年科学基金(批准号: 11305097, 11301318)、陕西省教育厅基金(批准号: 2013JK0616)和陕西理工学院人才启动基金(批准号: SLGQD13-23)资助的课题.

Authors and contacts

1.
School of Mathematics and Computer Science, Shaanxi University of Technology, Hanzhong 723000, China

Funds: Project supported by the Young Scientists Fund of the National Natural Science Foundation of China (Grant Nos. 11305097, 11301318), the education department of Shaanxi province of China (Grant No. 2013JK0616), and the Foundation of Shaaxi University of Technology of China (Grant No. SLGQD13-23).

参考文献

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[15]	Gregory R, Kanno S, Soda J 2009 J. High Energy Phys. 10 010
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[18]	Horowitz G T, Way B 2010 J. High Energy Phys. 1011 011
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[32]	Yan P, Pan Q Y, Wang B 2011 Phys. Lett. B 699 383
[33]	Yan Peng, Pan Q Y 2014 J. High Energy Phys. 06 011
[34]	Cai R G, He S, Li L, Li L F 2012 J. High Energy Phys. 1210 107
[35]	Brihaye Y, Hartmann B 2011 Phys. Rev. D 83 126008

施引文献

[1]	Maldacena J, Adv 1998 Theor. Math. Phys. 2 231; 1999 Int. J. Theor. Phys. 38 1113
[2]	Gubser S S, Klebanov I R, Polyakov A M 1998 Phys. Lett. B 428 105
[3]	Witten E, Adv 1998 Theor. Math. Phys. 2 253
[4]	Hartnoll S A 2009 Class. Quant. Grav. 26 224002
[5]	Herzog C P 2009 J. Phys. A 42 343001
[6]	Horowitz G T 2010 arXiv: 1002.1722 [hep-th]
[7]	Gubser S S 2008 Phys. Rev. D 78 065034
[8]	Gubser S S, Herzog C P, Pufu S S, Tesileanu T 2009 Phys. Rev. Lett. 103 141601
[9]	Liu Y Q, Pan Q Y, Wang B 2011 Phys. Lett. B 702 94
[10]	Gauntlett J P, Sonner J, Wiseman T 2009 Phys. Rev. Lett. 103 151601
[11]	Jing J L, Chen S B 2010 Phys. Lett. B 686 68
[12]	Pan Q Y, Wang B 2010 Phys. Lett. B 693 159
[13]	Nishioka T, Ryu S, Takayanagi T 2010 J. High Energy Phys. 03 131
[14]	Hartnoll S A, Herzog C P, Horowitz G T 2008 J. High Energy Phys. 12 015
[15]	Gregory R, Kanno S, Soda J 2009 J. High Energy Phys. 10 010
[16]	Pan Q Y, Wang B, Papantonopoulos E, Oliveria J, Pavan A B 2010 Phys. Rev. D 81 106007
[17]	Ge X H, Wang B, Wu S F, Yang G H 2010 J. High Energy Phys. 08 108
[18]	Horowitz G T, Way B 2010 J. High Energy Phys. 1011 011
[19]	Chen S B, Pan Q Y, Jing J L 2012 Chin. Phys. B 21 040403
[20]	Horowitz G T, Roberts M M 2008 Phys. Rev. D 78 126008
[21]	Cai R G, Zhang H Q 2010 Phys. Rev. D 81 066003
[22]	Jing J, Wang L, Chen S, arXiv:1001.1472
[23]	Setare M R, Momeni D 2011 J. High Energy Phys. 05 118
[24]	Ge X H, Wang B, Wu S F, Yang G H 2010 J. High Energy Phys. 1008 108
[25]	Maeda K, Natsuume M, Okamura T 2010 Phys. Rev. D 81 026002
[26]	Motull M, Pomarol A, Silva P J 2009 Phys. Rev. Lett. 103 091601
[27]	Albash T, johnson C V, 2009 Phys. Rev. D 80 126009
[28]	Brihaye Y, Hartmann B 2010 Phys. Rev. D 81 126008
[29]	Franco S, Garcia-Garcia A M, Rodriguez-Gomez D 2010 J. High Energy Phys. 1004 092
[30]	Franco S, Garcia-Garcia A M, Rodriguez-Gomez D 2010 Phys. Rev. D 81 041901
[31]	Peng Y, Pan Q Y 2013 Commun. Theor. Phys. 59 110
[32]	Yan P, Pan Q Y, Wang B 2011 Phys. Lett. B 699 383
[33]	Yan Peng, Pan Q Y 2014 J. High Energy Phys. 06 011
[34]	Cai R G, He S, Li L, Li L F 2012 J. High Energy Phys. 1210 107
[35]	Brihaye Y, Hartmann B 2011 Phys. Rev. D 83 126008

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