Logarithmic Corrections to the Entropy of Scalar Field in BTZ Black Hole Space-time

Logarithmic Corrections to the Entropy of Scalar Field in BTZ Black Hole Space-time

Dharm Veer Singh111Present Address: Centre for Theoretical Physics, Jamia Millia Islamia, New Delhi and Shobhit Sachan222Present Address: Government Engineering College, Mainpuri. Physics Department, Centre of Advanced Studies,
Banaras Hindu University, Varanasi - 221 005, (U.P.), India
e-mails: veerdsingh@gmail.com, shobhitsachan@gmail.com

The entanglement entropy correlates two quantum sub-systems which are the part of the larger system. A logarithmic divergence term present in the entanglement entropy is universal in nature and directly proportional to the conformal anomaly. We study this logarithmic divergence term of entropy for massive scalar field in dimension by applying numerical techniques to entanglement entropy approach. This (2+1) dimensional massive theory can be obtained from (3+1) dimensional massless scalar field via dimensional reduction. We also calculated mass corrections to entanglement entropy for scalar field. Finally, we observe that the area law contribution to the entanglement entropy is not affected by this mass term and the universal quantities depends upon the basic properties of the system.

I Introduction

Black holes are gravitational solutions of Einstein’s field equations. Black holes have some properties similar to that of a thermodynamical system. Therefore, like a thermodynamical system, entropy and temperature can be assigned to black holes. The temperature of a black hole is directly proportional to surface gravity of the event horizon.The entropy, known as Bekenstein-Hawking entropy is directly proportional to the area of the event horizonJD1 (); JD2 (); JD3 (); JD4 (); SWH ().

There are many attempts made to understand the origin of the black hole entropy. Some of the examples of these attempts are based on the calculation of a) the value of Euclidean action 7 (); 8 (); 10 (), b) the rate of the pair creation of black holes 11 (), c) the Noether charge of the bifurcate Killing horizon 13 (); 14 () and d) the central charge of the Virasoro algebra 15 (); 16 (); 17 ().

The microscopic derivation of the black hole entropy was given in superstring theory d1 (); d2 () by using the so-called D-brane method dbrane (); d3 (); d4 (). In 1985, ‘t Hooft introduced another model to calculate the entropy of a black hole, known as the brick wall model thooft (). Beside of all these previously well studied models, we concentrate our study on the entanglement entropy model Bombelli (); 19 (); 20 (); 21 (); 22 (); 23 (); 24 (); 25 (); Cadoni:2007vf (); Cadoni:2009tk (); Cadoni:2010vf (); Hung:2011ta () as this is the most attractive candidate for the black hole entropy.

The entanglement entropy is the source of quantum information. It is a measure of the correlation between subsystems, separated by a boundary called the entangling surface Bombelli (); 19 (). It is also a measure of the information loss due to division of the system. The entanglement entropy depends upon the geometry of the boundary, but not on the properties of the subsystems. The entanglement entropy is defined by the von Neumann entropy.

We study the logarithmic contribution to the entropy for scalar fields by using the dimensional reduction technique. In this technique, the coefficient of logarithmic divergence term in (2+1) dimensional massive theory can be obtained via dimensional reduction of (3+1) dimensional massless theory () using the entanglement entropy method. The reduced density matrix, which arises in the formulation, are written in terms of correlators Casini:2009sr (). The reduced density matrix in terms of correlators is well known for scalar fields and obeys the Wick’s theorem. The logarithmic divergence terms in entropy of black holes appear due to the infinite number of states near the horizon and these divergences scaled by the size of the black holes. These logarithmic divergence terms are related to the conformal anomalies. In even dimensions, conformal field theory (CFT) contains a divergence term, but in odd dimensions there is no divergence term across the entangling surface MPH (); Hertzberg:2012mn (). The coefficient of logarithmic term is proportional to the conformal anomaly SOLO1 () ( and type anomaly). For a spherical system, the results of “” type anomaly can be extended in any dimension Myers1 (); Hung:2011xb (), but “” type anomaly can not be extended in higher dimensional theory SOLO2 ().

This paper is organized as follows; we have given brief review of free massive theory in Sec. 2. We study the scalar field in BTZ black hole space-time in Sec. 3 and numerical calculations for logarithmic contribution to the entanglement entropy in Sec. 4. We present our results and their physical implication of entropy for scalar fields in BTZ black hole space-time in Sec 5. Some formulas which are used in the text, are defined in Appendix A.

Ii Free Massive Theory in BTZ Space-Time

The general structure of entanglement entropy of the system with logarithmic divergence is given by the relation,


where is the coefficient of the logarithmic divergence term and is the ultraviolet cutoff. The first part, which is finite, is Bekenstein-Hawking area law and second one is logarithmically divergence term of the entanglement entropy. For general conformal field theories in dimensions, the logarithmically divergence term is directly related to the and conformal anomalies. The relation between logarithmically divergence term and and type of anomalies is givenH2 (),


where is the Euler number of the surface where is radius of the cylinder). The is the extrinsic curvature, (with ) are the pair of unit vector orthogonal to , and is the induced metric on the surface. From equation (2), we can see that the coefficient of the logarithmic divergence of the cylinder is proportional to the type anomaly and is given by,


where and are the radius and length of the of the cylinder. Let us consider a system of three spatial dimensions of the form . The direction can be compactified by imposing the boundary conditions and thus the system reduces to two dimensions. The Fourier decomposition of the corresponding field modes in the compactified direction is given by,


This decomposition of fields enable us to write the EOMs in form,




In above definition, is the mass of the free fields and acts as infrared correlator and is an azimuthal quantum number. In our study, we consider the free massless field, therefore we set . In this case, the equation (6) becomes Safdi1 (); Safdi2 (),


The contribution of entanglement entropy of the two dimensional fields is given by the relation H2 (),


We expand in terms of and neglect higher order terms, obtaining the relation,


Substituting the value of in equation (8), we obtain the the logarithmic coefficient in which is directly related to by the relation,


The coefficient is obtained from the free massless theory in (3+1) dimensions and is directly related to the coefficient of . The coefficient is found for scalars.

Now, The logarithmic divergence term of entropy is proportional to the mass term in the dimensionally reduced theory and given by the term . The entropy of scalar field is given by MPH (),


where and “” is the area of event horizon . For , the value of is . The coefficient is linear with entropy and it is found .

Iii Scalar Fields in BTZ Black Hole Space-time

Let us consider the action of the (2+1) dimensional gravity with cosmological constant MB (); Carlip (),


The value of cosmological constant is . One of the solution of this dimensional gravity with negative cosmological constant is is BTZ black hole. The metric of BTZ black hole is given by the equation;


where and . The metric of the BTZ black hole in term of proper distance is written as,


Where and and are inner and outer horizon of the black hole respectively.

The action of massive scalar field in the background of BTZ black hole is written as,


where and are the determinant and the metric element of the BTZ black hole (14). The field can be decomposed using the separation of variables . This decomposition of manifest the cylindrical symmetry of the system. Substituting the value of and in equation (15), we get the expression,


where is the conjugate momentum corresponding the field . The Hamiltonian of the scalar field in the BTZ background space-time is given by DS1 (); DS2 (); DS3 (),


This Hamiltonian is not diagonal, therefore to diagonalize it, we define the new momentum . The canonical variables, the field () and diagonalized momentum () satisfy the following relation,


Using the diagonalized momentum, the diagonalized Hamiltonian can be written as DS1 (); DS2 (); DS3 (),




For general quadratic case, the Hamiltonian of the system is written as,


where and obey the commutation relation and is the matrix. The two point correlator is given by,


where and are defined in appendix (A). Then the entropy of the system is given by the relation




We make the following replacements to discretized the Hamiltonian of the system,

where and “” is the lattice spacing . We discretized Hamiltonian (19) using the above replacements and we suppressed the angular momentum index . The matrix elements corresponding to the discretized Hamiltonian (19) is given by, 333We discretized the Hamiltonian (19) using the the middle-point prescription and the derivative of the form is replaced by ,


The diagonal and off-diagonal terms are given by,


where and “” is UV cut-off length. We regain the continuum by taking the limit and while the size of the system remains fixed.

Iv Numerical Estimation

In this section, we study the numerical estimation of entanglement entropy of massive scalar field in BTZ black hole space time. We start from with the calculation of matrix of , where for given mass and angular momentum . We calculate the correlator and and then calculate the entropy of massive field in BTZ black hole space-time. For the numerical computation, we consider the system is discretized in radial direction with lattice size and the partition size .

The entropy can be expanded in powers of proper distance, , for large values of ,


The entropy of scalar field for different masses in the range is computed numerically. The Value of and are tabulated in the table (1),

   0.401 0.354    0.302    0.241    0.204
      0.200 0.068    0.050    0.040    0.030
Table 1: The value of and for different masses 0.1, 0.2, 0.3, 0.4 and 0.5.

The value of coefficients and are tabulated in the table (1) and shown in figure (1). If we calculated the value of coefficients, then we expand the and in power of M,

Figure 1: The numerical calculation for of the scalar field in rotating BTZ space-time. is shown as a functions of for different masses m=0.1, 0.3 and 0.5 . We have taken the lattice point N=200.

The plot and as the coefficient of and in (29) and (30). The value of and as shown in figure (2) and (3). The co-efficients and are found from the fitting the data plotted in figure (3) and the values are -0.503 and -0.0132 respectively. Here it is interesting to note that the co-efficients is related with the co-efficient of logarithmic term in (3+1) dimension and is given by and for the co-efficients (is obtained from dimensionally reduced theory ) is given by .

Figure 2: The points corresponds to the coefficient of the linear term in r in the entanglement entropy for different masses.
Figure 3: The points corresponds to the coefficient of the term in the entanglement entropy for different masses.The coefficient of term is proportional to 1/M in the fit drawn with a solid line is 0.0132 = /240. This is the value of in equation (5.22).

V Conclusion

In this paper, we have studied the logarithmic divergence term of entanglement entropy for the scalar field propagating in the background of BTZ black hole numerically. The coefficient of divergence term and calculated numerically. The logarithmic divergence term(s) of entanglement entropy is the linear combination of type anomaly. The term is obtained from the dimensional reduction of the theory and the term is directly related to the coefficient of divergence term. The general structure of the coefficients is same as that found in (8). This is the agreement of our numerical results with analytical results MPH (). We can also extend our results for the higher dimension theory. We have also studied the logarithmic divergence term of entanglement entropy for the fermion field propagating in the background of BTZ black hole numerically DS4 ().

Appendix A Model of entanglement Entropy

In this appendix, the model of entanglement entropy for scalar field and numerical computation of entropy is reviewed. Let there is a system of coupled harmonic oscillators which one can use to study the entanglement entropy of the system. The Hamiltonian of this coupled harmonic oscillator system is written as,


Where and are canonical momentum corresponding to the and respectively. Tha canonical momenta are given by the relation , where is Kronecker delta, is real, symmetric, positive definite matrix and “a” is fundamental length characterizing the system. Using the creation and annihilation operators, one can write total Hamiltonian as,


where is symmetric, positive definite matrix satisfying the condition . Operators and are annihilation and creation operators respectively, similar to that of harmonic oscillator problem and they obey similar commutation relation,


If is the ground state for the harmonic oscillator system, then it follows the condition


and the solution is given by, Bombelli ()


The density matrix of the ground state is obtained by


We split into two subsystems, and 444The subsystem and subsystem regards as the inside and outside mode of the horizon. The reduced density matrix of the subsystem “1” is obtained by tracing the degrees of freedom of the subsystem “2” 555The subsystem “1” and subsystem “2” refers to the subsystem with label “” and subsystem with label “” respectively. , and is given by;


The matrix W naturally splits into four blocks asDS2 (); DS3 (); DS4 (),

Now we find that reduced density matrix can be written as,




The reduced density matrix of the system ‘1’ is obtained by tracing the degrees of freedom of the system ‘2’ and is same as above equation (38). The system can be diagonalized by the unitary matrix and the transformations


Thus the density matrix reduces to Bombelli (),


where are the eigenvalues of the matrix . The entropy of the system can be calculated by the relation (25).


I would like to thank Dr. Sanjay Siwach for useful discussions. The work of Dharm Veer Singh is supported by Rajiv Gandhi National Fellowship Scheme of University Grant Commission (Under the fellowship award no. F.14-2(SC)/2008 (SA-III)) and of Shobhit Sachan is supported by Council of Scientific and Industrial Research (CSIR) (Under the fellowship award no. 09/013(0239/2009-EMR-1)) of Government of India.


  • (1) J. D.  Bekenstein, Phy. Rev. D 7, 2333 (1973).
  • (2) J. D.  Bekenstein, ‘ Lett. al Nuovo Ciemnto 4 (1972) 15.
  • (3) J. D.  Bekenstein, Phy. Rev. D 9, 3292 (1974).
  • (4) J. D.  Bekenstein, Phy. Rev. D 12, 3077 (1975).
  • (5) S. W. Hawking, Phy. Rev. D 13, 191 (1976).
  • (6) G. W. Gibbons and S. W. Hawking, Phys. Rev. D 15, 2752 (1977).
  • (7) J. D. Brown and J. W. York, Jr., Phys. Rev. D 47, 1420 (1993) [gr-qc/9209014].
  • (8) S. W. Hawking and C. J. Hunter, Phys. Rev. D 59, 044025 (1999) [hep-th/9808085].
  • (9) D. Garfinkle, S. B. Giddings and A. Strominger, Phys. Rev. D 49, 958 (1994) [gr-qc/9306023].
  • (10) R. M. Wald, Phys. Rev. D 48, no. 8, R3427 (1993) [gr-qc/9307038].
  • (11) V. Iyer and R. M. Wald, Phys. Rev. D 50, 846 (1994) [gr-qc/9403028].
  • (12) S. Carlip, Phys. Rev. D 51, 632 (1995) [gr-qc/9409052].
  • (13) A. Strominger, JHEP 9802, 009 (1998) [hep-th/9712251].
  • (14) S. Carlip, Phys. Rev. Lett. 82, 2828 (1999) [hep-th/9812013].
  • (15) M. B. Green, J. H. Schwarz and E. Witten, “Superstring Theory. Vol. 1 & 2,” Cambridge, Uk: Univ. Pr. ( 1987). ( Cambridge Monographs On Mathematical Physics).
  • (16) J. Polchinski, “String theory. Vol. 1 & 2,” (Cambridge University Press 1998).
  • (17) J. Polchinski, S. Chaudhuri and C. V. Johnson, “Notes on D-branes,” hep-th/9602052.
  • (18) A. Strominger and C. Vafa, Phys. Lett. B 379, 99 (1996) [hep-th/9601029].
  • (19) J. M. Maldacena, hep-th/9607235.
  • (20) G. ’tHooft, Nucl. Phys. B 256, 727 (1985).
  • (21) L. Bombelli, R. K. Koul, J. Lee and R. D. Sorkin, Phys. Rev. D 34, 373 (1986).
  • (22) M. Srednicki, Phys. Rev. Lett. 71, 666 (1993) [hep-th/9303048].
  • (23) V. P. Frolov and I. Novikov, Phys. Rev. D 48, 4545 (1993) [gr-qc/9309001].
  • (24) C. G. Callan, Jr. and F. Wilczek, Phys. Lett. B 333, 55 (1994) [hep-th/9401072].
  • (25) D. N. Kabat and M. J. Strassler, Phys. Lett. B 329, 46 (1994) [hep-th/9401125].
  • (26) C. Holzhey, F. Larsen and F. Wilczek, Nucl. Phys. B 424, 443 (1994) [hep-th/9403108].
  • (27) S. Mukohyama, M. Seriu and H. Kodama, Phys. Rev. D 55, 7666 (1997) [gr-qc/9701059].
  • (28) S. Mukohyama, M. Seriu and H. Kodama, Phys. Rev. D 58, 064001 (1998) [gr-qc/9712018].
  • (29) M. Cadoni, Phys. Lett. B 653 (2007) 434, arXiv:0704.0140 [hep-th].
  • (30) M. Cadoni and M. Melis, Found. Phys. 40 (2010) 638, arXiv:0907.1559 [hep-th].
  • (31) M. Cadoni and M. Melis, Entropy 2010, 12, 2244-2267.
  • (32) L. -Y. Hung, R. C. Myers and M. Smolkin, JHEP 1108 (2011) 039, arXiv:1105.6055 [hep-th].
  • (33) H. Casini and M. Huerta, J. Phys. A 42, 504007 (2009), arXiv:0905.2562 [hep-th]
  • (34) M. P. Hertzberg and F. Wilczek, Phys. Rev. Lett. 106, 050404 (2011), arXiv:1007.0993 [hep-th].
  • (35) M. P. Hertzberg J. Phys. A 46, 015402 (2013), arXiv:1209.4646 [hep-th].
  • (36) S. N. Solodukhin, Phys. Lett. B 665 (2008) 305, arXiv:0802.3117 [hep-th].
  • (37) H. Casini, M. Huerta and R. C. Myers, JHEP 1105 (2011) 036, arXiv:1102.0440 [hep-th]
  • (38) L. -Y. Hung, R. C. Myers and M. Smolkin, JHEP 1104 (2011) 025, arXiv:1101.5813 [hep-th].
  • (39) S. N. Solodukhin, Living Rev. Rel. 14 (2011) 8, arXiv:1104.3712 [hep-th].
  • (40) M. Huerta, Phys. Lett. B 710 (2012) 691, arXiv:1112.1277 [hep-th].
  • (41) Igor R. Klebanov, Tatsuma Nishioka, Silviu S. Pufu, Benjamin R. Safdi JHEP 1207 (2012) 001, arXiv:1204.4160 [hep-th].
  • (42) B. R. Safdi, JHEP 1212 (2012) 005, arXiv:1206.5025 [hep-th].
  • (43) Maximo Banados, Claudio Teitelboim and Jorge Zanelli, Phy. Rev. Lett. 69(1992) 1849.
  • (44) S. Carlip, Class. Quantum Gravity 12(1995) 2853, arXiv:9506079v1 [gr-qc].
  • (45) Dharm Veer Singh and Sanjay Siwach Class. Quantum Grav. 30 (2013) 235034, arXiv: 1106.1005 [hep-th].
  • (46) Dharm Veer Singh and Sanjay Siwach Journal of phys. Conf. Series 481 (2014) 012014.
  • (47) Dharm Veer Singh Int. J. Mod. Phys. D 24:1550001, arXiv: 1406.3809 [hep-th].
  • (48) Dharm Veer Singh and Sanjay Siwach; Advances in High Energy Physics, Volume 2015 (2015), Article ID 528762, arXiv: 1406.3799 [hep-th].
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