Deconfinement phase transition in a magnetic field in 2+1 dimensions from holographic models

Deconfinement phase transition in a magnetic field in 2+1 dimensions from holographic models

Abstract

Using two different models from holographic quantum chromodynamics (QCD) we study the deconfinement phase transition in dimensions in the presence of a magnetic field. Working in 2+1 dimensions lead us to exact solutions on the magnetic field, in contrast with the case of 3+1 dimensions where the solutions on the magnetic field are perturbative. As our main result we predict a critical magnetic field where the deconfinement critical temperature vanishes. For weak fields meaning we find that the critical temperature decreases with increasing magnetic field indicating an inverse magnetic catalysis (IMC). On the other hand, for strong magnetic fields we find that the critical temperature raises with growing field showing a magnetic catalysis (MC). These results for IMC and MC are in agreement with the literature.

I Introduction

The deconfinement phase transition in quantum chromodynamics (QCD) still remains an open and intriguing problem, since the standard perturbative method does not work due to the strong coupling regime at low energies. The usual approach to deal with this non-perturbative issue is lattice QCD where one finds a critical temperature which characterises the deconfinement phase transition. In particular, the presence of a magnetic field modifies this scenario. It has been shown recently Bali:2011qj () that weak magnetic fields imply a decreasing , an effect known as inverse magnetic catalysis (IMC). Furthermore, it is expected that for strong magnetic fields increases with , meaning a magnetic catalysis (MC). The MC/IMC studies are usually concerned with chiral symmetry breaking and/or deconfinement phase transition.

Currently, many works have dealt with MC/IMC using a holographic approach based on the AdS/CFT correspondence. This correspondence or duality makes it possible to relate strong coupling theory in flat Minkowski space with weak coupling supergravity in anti-de Sitter space (AdS) in a higher dimensional space Maldacena:1997re (); Gubser:1998bc (); Witten:1998qj (). Among these works we can mention Evans:2010xs (); Alam:2012fw (); Filev:2010pm (); Callebaut:2011zz (); Bolognesi:2011un () where they study the MC problem, while Preis:2010cq (); McInnes:2015kec (); Evans:2016jzo (); Mamo:2015dea (); Li:2016gfn (); Dudal:2015wfn () discuss IMC effects in different holographic models. Note that in all of these 3+1 dimensional models the gravitational solutions on the magnetic field are perturbative.

Here in this work we study deconfinement phase transition in 2+1 dimensions in the presence of an external magnetic field within two different holographic AdS/QCD models. We find the IMC and MC pictures for the deconfinement phase transition and obtain an intriguing critical magnetic field for which the critical temperature vanishes. The advantage of working in 2+1 dimensions is that the system of equations are simpler than the 3+1 dimensional case, leading us to some exact solutions where we can obtain the IMC/MC transition at a critical value of =. In ref. Bolognesi:2011un () the case of 2+1 dimensions was studied for the case of the MC on the fermion condensate.

The holographic models that we use are known as the hard Polchinski:2001tt (); BoschiFilho:2002vd () and soft wall Karch:2006pv (); Colangelo:2007pt (). Such models were successful in predicting the deconfinement phase transition and its critical temperature in the absence of a magnetic field Herzog:2006ra (); BallonBayona:2007vp (). These holographic models appeared after the proposal of the AdS/CFT correspondence, which provides an approach to deal problems out of the perturbative regime of QCD or other strongly interacting systems.

This work is organized as follows: in section II we review the Einstein-Maxwell Theory in 4 dimensions and the geometric set up in the presence of an external magnetic field. In section III we describe the holographic models used and compute the corresponding on-shell actions for both thermal and black hole AdS spaces. Then, in section IV, we present our results for the deconfinement phase transition in the hard and soft wall models in the presence of an external magnetic field and obtain the critical magnetic field . Finally, in section V we present our last comments and conclusions.

Ii Einstein-Maxwell Theory in 4 dimensions

Here, we start with holographic models defined in such that the dual field theory in Euclidean space lives in 3 dimensions. The full gravitational background is the eleven-dimensional supergravity on . The dual field theory is the low-energy theory living on -branes on , with Super-Yang-Mills theory in the large limit Aharony:1999ti (). Via Kaluza-Klein dimensional reduction, the supergravity theory on may be consistently truncated to Einstein-Maxwell Theory on Herzog:2007ij (). The action for this theory, in Euclidean signature is given by

(1)

where is the 4-dimensional coupling constant, which is proportional to the 4-dimensional Newton’s constant , is the Ricci scalar and is the negative cosmological constant which, for , are given by , and , respectively. is the radius of and is the Maxwell field. The second integral corresponds to the surface and counter-terms in which is the determinant of the induced metric on the boundary, and is the trace of the extrinsic curvature which gives the Gibbons-Hawking surface term Gibbons:1976ue (). The last term is a counter-term needed to cancel the UV divergences () of the bulk action.

The field equations coming from the bulk action (1) are Herzog:2007ij ()

(2)

together with the Bianchi identities . The ansatz for the metric to solve these equations is given by

(3)

in Euclidean signature with a compact time direction, , with , and is a function to be determined in the following. The background magnetic field is chosen such that , which implies . Note that the magnetic field remains finite at the boundary (). To see this let’s consider the vector potential, which is a 1-form such that . So, . Thus, we can treat it as an external background magnetic field Hartnoll:2007ai ().

Using the ansatz (3) the field equations (2) are simplified and given by

(4)
(5)

The two exact solutions of (4) that we found are given by

(6)
(7)

The first solution, , corresponds to the thermal with an external background magnetic field. The second solution, , corresponds to a black hole in also in the presence of a background magnetic field, and where is the horizon position, such that . One can note the these two solutions indeed satisfy both differential equations (4). This is in contrast with the 3+1 dimensional case where only perturbative solutions on the magnetic field are found.

Iii On-shell Euclidean Actions

iii.1 Hard wall

The hardwall model Polchinski:2001tt (); BoschiFilho:2002vd () consists in introducing a hard cut-off in the background geometry in order to break conformal invariance. The introduction of a cut-off in this model implies that , where can be related to the mass scale of the boundary theory. For instance, in dimensions is usually related with energy scale of QCD BoschiFilho:2005yh (); Rodrigues:2016cdb () by . Moreover we have to impose boundary conditions in .

In the hard wall model, the free energy for the thermal AdS, from the action (1), is given by (see DCB2017 () for details):

(8)

where , is the corresponding period, and is an UV regulator.

On the other hand, for the black hole case one gets the free energy

(9)

where is associated with the Hawking temperature.

Now we have to compute the free energy difference, , defined by . Since we are comparing the two geometries at the same position we can choose such that Herzog:2006ra (); BallonBayona:2007vp (), since when , with given by the second equation in (6). Therefore, with this choice, we have that the free energy difference for the hardwall model is given by

(10)

For , this equation corresponds to the 3-dimensional version of Herzog:2006ra ().

iii.2 Soft wall

For the soft wall model Colangelo:2007pt (); Karch:2006pv () we consider the following 4-dimensional action

(11)

where is the dilaton field, which has non-trivial expectation value. In this work we are assuming that the dilaton field does not backreact on the background geometry. Moreover, as in Herzog:2006ra (), we assume that our metric ansatz (3) satisfies the equations of motion for the full theory with given by (6) for both thermal and black hole in . One can note that we included one more term on the boundary action compared to (1), due to the dilaton field in this soft wall model.

The free energy for the thermal , in the soft wall model is given by

(12)

On the other hand, the free energy for the black hole for the soft wall model, is

(13)

where is the error function.

Therefore, taking into account the same argument which led to in the hardwall model, the free energy difference, , for the softwall model is given by

(14)

where erfc is the complementary error function, defined as .

Iv Deconfinement Phase Transition

Following Hawking and Page Hawking:1982dh () and Witten Witten:1998zw (), we study the deconfinement phase transition imposing where is the critical horizon, from which we calculate the critical temperature through the formula where is the horizon function given by (6).

In the hard wall model with and from (10) we find that the deconfinement phase transition occurs at resulting in the critical temperature , which is the analogue in dimensions of Herzog:2006ra (); BallonBayona:2007vp (). In order to fix the cut off we use Neumann boundary condition which gives so that , where is the lightest scalar glueball mass = 4.37 for SU(3) in (2+1) dimensions where is the string tension Teper:1998te (); Athenodorou:2016ebg (). Then, one can compute and the critical temperature, , in units of the string tension for :

(15)

For the soft wall model, for , there is a phase transition when which gives the critical temperature consistent with the treatment presented in Herzog:2006ra (); BallonBayona:2007vp () for in one higher dimension. In order to fix the value of we consider the soft wall model in 4 dimensions so that we have (see DCB2017 () for details). Using the mass for the lightest glueball in dimensions from the lattice Athenodorou:2016ebg () and setting , we can fix the dilaton constant 3.18 for the SU(3), in units of the string tension squared. Therefore, the critical temperature, , in units of the string tension, is given by

(16)

On the other hand, for from (10) (hard wall), and (14) (soft wall), the numerical results for the critical temperature as a function of the magnetic field, , is shown in Figure 1, for both models. One can see from this figure that we have a phase in which the critical temperature, , decreases with increasing magnetic field , indicating an inverse magnetic catalysis (IMC). Furthermore, we also predict a phase in which the critical temperature, , increases with increasing magnetic field , indicating a magnetic catalysis (MC).

The magnetic and inverse magnetic catalysis we have found for these models are separated by a critical magnetic field, . The values of the critical magnetic fields found in these models, in units of the string tension squared, are the following

(17)
(18)

In Figure 2 we show the plot of the normalized critical temperature, , as a function of for both models, where and is the critical magnetic field (17), and (18).

Figure 1: Critical temperature (in units of string tension) as a function of the magnetic field (in units of string tension squared).
Figure 2: The ratio of the critical temperatures as a function of the ratio of the magnetic fields.

V Discussions

The IMC has been observed in lattice QCD Bali:2011qj () for 1 GeV. Since then many holographic approaches reproduced this behavior in both deconfinement and chiral phase transition contexts within this range of magnetic field, see for instance Mamo:2015dea (); Dudal:2015wfn (); Evans:2016jzo (); Li:2016gfn ().

However, in many of these approaches the problem could only be solved perturbatively in , while in our results in (2+1) dimensions there is no restriction for the values or range of the magnetic field. This is in contrast with the 3+1 dimensional case where only perturbative solutions on the magnetic field are found. Since we are working in dimensions, physical quantities such as the critical temperature, , magnetic field, , and critical magnetic field, , are not measured in GeV or MeV. Instead we used the string tension as the basic unit for our physical quantities, as is the case in lattice simulations Athenodorou:2016ebg (); Teper:1998te (); Meyer:2003wx ().

In conclusion, we emphasize that the critical magnetic field found here is an unexpected result since in 3+1 dimensional QCD there is evidence that the deconfinement (and chiral) transition is a cross over Bali:2011qj ().

Acknowledgments: We would like to thank Luiz F. Ferreira, Adriana Lizeth Vela, Renato Critelli, Rômulo Rogeumont, and Marco Moriconi for helpful discussions during the course of this work. We also thank Elvis do Amaral for the help with numerical solutions. We would also like to thank Michael Teper for useful correspondence. D.M.R is supported by Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), E.F.C. is partially supported by PROPGPEC-Colégio Pedro II, and H.B.-F. is partially supported by CNPq.

References

  1. G. S. Bali, F. Bruckmann, G. Endrodi, Z. Fodor, S. D. Katz, S. Krieg, A. Schafer and K. K. Szabo, JHEP 1202, 044 (2012) [arXiv:1111.4956 [hep-lat]].
  2. J. M. Maldacena, Int. J. Theor. Phys. 38, 1113 (1999) [Adv. Theor. Math. Phys. 2, 231 (1998)] [hep-th/9711200].
  3. S. S. Gubser, I. R. Klebanov and A. M. Polyakov, Phys. Lett. B 428, 105 (1998) [hep-th/9802109].
  4. E. Witten, Adv. Theor. Math. Phys. 2 (1998) 253 [hep-th/9802150].
  5. N. Evans, T. Kalaydzhyan, K. y. Kim and I. Kirsch, JHEP 1101, 050 (2011) doi:10.1007/JHEP01(2011)050 [arXiv:1011.2519 [hep-th]].
  6. M. S. Alam, V. S. Kaplunovsky and A. Kundu, JHEP 1204, 111 (2012) [arXiv:1202.3488 [hep-th]].
  7. V. G. Filev and R. C. Raskov, Adv. High Energy Phys. 2010, 473206 (2010) [arXiv:1010.0444 [hep-th]].
  8. N. Callebaut, D. Dudal and H. Verschelde, Acta Phys. Polon. Supp. 4, 671 (2011).
  9. S. Bolognesi and D. Tong, Class. Quant. Grav. 29 (2012) 194003 [arXiv:1110.5902 [hep-th]].
  10. F. Preis, A. Rebhan and A. Schmitt, JHEP 1103, 033 (2011) [arXiv:1012.4785 [hep-th]].
  11. B. McInnes, Nucl. Phys. B 906, 40 (2016) [arXiv:1511.05293 [hep-th]].
  12. N. Evans, C. Miller and M. Scott, Phys. Rev. D 94, no. 7, 074034 (2016) [arXiv:1604.06307 [hep-ph]].
  13. K. A. Mamo, JHEP 1505, 121 (2015) [arXiv:1501.03262 [hep-th]].
  14. D. Li, M. Huang, Y. Yang and P. H. Yuan, JHEP 1702, 030 (2017) [arXiv:1610.04618 [hep-th]].
  15. D. Dudal, D. R. Granado and T. G. Mertens, Phys. Rev. D 93, no. 12, 125004 (2016) [arXiv:1511.04042 [hep-th]].
  16. J. Polchinski and M. J. Strassler, Phys. Rev. Lett. 88, 031601 (2002) [arXiv:hep-th/0109174].
  17. H. Boschi-Filho and N. R. F. Braga, JHEP 0305, 009 (2003) [arXiv:hep-th/0212207].
  18. A. Karch, E. Katz, D. T. Son and M. A. Stephanov, Phys. Rev. D 74, 015005 (2006) [hep-ph/0602229].
  19. P. Colangelo, F. De Fazio, F. Jugeau and S. Nicotri, Phys. Lett. B 652, 73 (2007) [hep-ph/0703316].
  20. C. P. Herzog, Phys. Rev. Lett. 98, 091601 (2007) [hep-th/0608151].
  21. C. A. Ballon Bayona, H. Boschi-Filho, N. R. F. Braga and L. A. Pando Zayas, Phys. Rev. D 77, 046002 (2008) [arXiv:0705.1529 [hep-th]].
  22. O. Aharony, S. S. Gubser, J. M. Maldacena, H. Ooguri and Y. Oz, Phys. Rept. 323, 183 (2000) [hep-th/9905111].
  23. C. P. Herzog, P. Kovtun, S. Sachdev and D. T. Son, Phys. Rev. D 75, 085020 (2007) [hep-th/0701036].
  24. G. W. Gibbons and S. W. Hawking, Phys. Rev. D 15, 2752 (1977).
  25. S. A. Hartnoll and P. Kovtun, Phys. Rev. D 76, 066001 (2007) [arXiv:0704.1160 [hep-th]].
  26. H. Boschi-Filho, N. R. F. Braga and H. L. Carrion, Phys. Rev. D 73, 047901 (2006) [hep-th/0507063].
  27. D. M. Rodrigues, E. Folco Capossoli and H. Boschi-Filho, Phys. Rev. D 95, no. 7, 076011 (2017) [arXiv:1611.03820 [hep-th]].
  28. D. M. Rodrigues, E. Folco Capossoli and H. Boschi-Filho, arXiv:1710.07310 [hep-th].
  29. S. W. Hawking and D. N. Page, Commun. Math. Phys. 87, 577 (1983).
  30. E. Witten, Adv. Theor. Math. Phys. 2, 505 (1998) [hep-th/9803131].
  31. M. J. Teper, Phys. Rev. D 59, 014512 (1999) [hep-lat/9804008].
  32. A. Athenodorou and M. Teper, JHEP 1702, 015 (2017) [arXiv:1609.03873 [hep-lat]].
  33. H. B. Meyer and M. J. Teper, Nucl. Phys. B 668, 111 (2003) [hep-lat/0306019].
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
214479
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description