Powerlaw corrections to blackhole entropy via entanglement
Abstract
We consider the entanglement between quantum field degrees of freedom inside and outside the horizon as a plausible source of blackhole entropy. We examine possible deviations of black hole entropy from area proportionality. We show that while the area law holds when the field is in its ground state, a correction term proportional to a fractional power of area results when the field is in a superposition of ground and excited states. We compare our results with the other approaches in the literature.
1 Introduction
It is now wellknown that the blackhole (commonly referred to as BekensteinHawking) entropy is finite and is given by the relation [1]
(1) 
is the area of the blackhole horizon. It is infinite, if both the matter and gravity are purely classical! In other words, the finiteness of the blackhole entropy (and the validity of secondlaw of thermodynamics) requires that the matter and(or) gravity to be quantized.
Although the above relation has been derived by various approaches [2, 3, 4, 5], we do not yet understand: Why is not extensive? What is the microscopic origin of blackhole entropy? Are there corrections to the BekensteinHawking entropy? and How generic are these corrections?
The purpose of this paper is an attempt to understand the generic corrections to the BekensteinHawking entropy by assuming entanglement as a source of blackhole entropy. We show that while the area law holds when the field is in its ground state, a correction term proportional to a fractional power of area results when the field is in a superposition of ground and excited states.
The paper is organized as follows: In the next section, we briefly discuss various properties of entanglement entropy and provide motivation for the relevance of the entanglement entropy to . In Sec. (3), we discuss the setup and the key steps in evaluating the entanglement entropy of scalar field propagating in flat spacetime. In Sec. (4), we obtain the entanglement entropy for a superposed state and show explicitly that the powerlaw corrections become important for small horizon limit. We conclude with a summary in Sec. (5). In appendix, we show explicitly that at a fixed Lemaitre time, the Hamiltonian of a scalar field in a black hole background reduces to that in flat spacetime.
2 Entanglement entropy
Let us consider a bipartite quantum system and assume that is in a pure state . The entanglement entropy () is defined as
(2) 
where
(3) 
is the Von Neumann entropy, are the Eigenvalues of obtained by solving the integral equation
(4) 
and
(5) 
is the reduced density matrix obtained by tracing over 2. Note that the entanglement entropy (2) is independent of the which degrees of freedom are traced over.
In order to set the ideas, we consider a simple example — 2coupled harmonic oscillator. The Hamiltonian of a coupled Harmonic oscillator is given by
(6) 
where are coordinate and momenta of the oscillator, respectively, and is the interaction term which is assumed to be positive. The quantization of the above Hamiltonian is straight forward in the normal coordinates:
(7) 
The ground state wave function is given by
where
(8) 
Let us consider the situation in which we choose not to have any information about the oscillator . Mathematically, this corresponds to tracing over the oscillator 1, i. e.,
(9)  
where
(10) 
Substituting (9) in the integral equation (4), the eigenfunctions and eigenvalues are given by
(11) 
Substituting the eigenvalues in (3), the entanglement entropy is given by
(12) 
In Fig. (1), we have plotted of the coupled oscillator in terms of . It is interesting to note that the entanglement entropy vanishes when the oscillators are uncoupled () while they diverge in the strongly coupled limit ().
But what has this digression to do with blackholes and what is the relevance of to blackhole entropy? This can be understood from the fact that both entropies are associated with the existence of the horizons. Consider a scalar field on a background of a collapsing star. At early times, there is no horizon, and both the entropies are zero. However, once the horizon forms, is nonzero, and if the scalar field degrees of freedom inside the horizon are traced over, obtained from the reduced density matrix is nonzero as well.
In the next section, we give the procedure for evaluating the entanglement entropy of quantum scalar field propagating in flat spacetime. In the Appendix, we have shown explicitly that at a fixed Lemaitre time, the Hamiltonian of a scalar field in Schwarzschild spacetime reduces to that in flat spacetime. All the results we derive in case of flat spacetime can then be extended to the blackhole spacetime at a fixed Lemaitre time.
3 Entanglement entropy for scalar fields – Setup
The Hamiltonian of a free massless scalar field propagating in the Minkowski spacetime is given by
(13) 
For simplicity, let us assume that the scalar field in confined in a spherical box . The cartoon version of the setup is provided in Fig (2).
Partialwave decomposition of the scalar field and its canonical conjugate
(14) 
leads to the following reduced Hamiltonian:
(15) 
where are the real Spherical harmonics. (For details, see Refs. [5, 6, 7].)
The computation of the entanglement entropy involves three steps: (i) Discretize the Hamiltonian, (ii) Choose a quantum state, and (iii) Trace over region 2 (or 1) to obtain the density matrix.
Note that, even if we obtain closedform expression of the density matrix, it is not possible to analytically evaluate the entanglement entropy. Hence, we need to resort to numerical methods. In the rest of the section, we discuss these steps in detail.
3.1 Discretized Hamiltonian
Discretizing the Hamiltonian (15) in a spherical lattice as described in Fig. (2), we get
(16)  
where is the lattice spacing, () is the length of the box, is the number of lattice points and the interaction matrix is given by
Note that the Hamiltonian (16) is a coupled Harmonic oscillators which satisfy the following commutation relations:
(17) 
3.2 Choice of quantum state
The general Eigen state of the coupled harmonic oscillators is
where is the diagonal matrix of obtained by the unitary transformation , is a unitary matrix and .
It is not possible to obtain a closed form expression for the density matrix for such a general state. To make the calculations tractable, we make two choices for the particle state:
3.3 Density matrix
For a general Eigen state, the physical operation of trace over region 2 ( oscillators) [cf. Fig. (2)] is given by
For the two special choices which we discussed in the previous subsection, the above expression reduces to

Vacuum state:
(20) which corresponds to product of 2coupled harmonic oscillators with 1 harmonic oscillator traced as discussed in Sec. (2).

1Particle state:
where
(21)
As mentioned earlier, it is not possible to evaluate the entanglement entropy analytically and we need to resort to numerical computations. We use Matlab to evaluate the entropy and the numerical error in our computation is less than .
In Fig. (3), we have plotted the entanglement entropy for the ground state and 1particle state for . We see that for the 1particle state, the entropy scales as , with lesser for higher . It is less than unity for any i. e., more the excitation, larger is deviation from area law The area law does not seem to hold! This implies that the entanglement entropy depends on the choice of the quantum state of the field.
4 Power law corrections to area
Given the above results, one may draw two distinct conclusions: first that entanglement entropy is not robust and reject it as a possible source of blackhole entropy. Second, since entanglement entropy for excited state scales as a lower power of area it is plausible that when a generic state (consisting of a superposition of ground state and excited state) is considered, corrections to the BekensteinHawking entropy will emerge. In order to determine which one is correct, it is imperative to investigate various generalizations of the scenarios considered in Ref. [5]. To this end, in this section we calculate the entanglement entropy of the mixed superposition of vacuum and 1particle state
(22) 
Following the procedure discussed in the previous section, it is possible to obtain the entanglement entropy of the superposed state. In Fig. (4) we have plotted the relative entropy [i.e ratio of the superposed and ground state entanglement entropy] for different values of and . From Fig. (4) it is easy to see that for large values of the horizon radius the entanglement entropy of the superposed state approaches the ground state entanglement entropy. In other words, for large horizon area, the entanglement entropy of the superposed state scales as area of the horizon.
In order to know the behavior of the entanglement entropy for the small horizon limit, in Fig. (5), we have obtained the best numerical fit for the relative entropy. From these, we see that the entanglement entropy of the superposed state is given by:
(23) 
where and are constants. This is the main result of this paper and we would like to stress the following points: (i) The second term in the above expression may be regarded as a power law correction to the area law, resulting from entanglement, when the wavefunction of the field is chosen to be a superposition of ground and excited states. (ii) It is important to note that the correction term falls off rapidly with (due to the negative exponent) and in the large area limit () the arealaw is recovered. This lends further credence to entanglement as a possible source of black hole entropy. (iii) The correction term is more significant for greater excited stateground state mixing proportion . For detailed discussion see Refs. [7, 8].
5 Conclusions
In this work, we have obtained powerlaw corrections to the BekensteinHawking entropy, treating the entanglement between scalar field degrees of freedom inside and outside the horizon as a viable source of blackhole entropy. We have shown that for small black hole areas the area law is violated when the oscillator modes are in a linear superposition of ground and excited states. We found that the corrections to the arealaw become increasingly significant as the proportion of excited states in the superposed state increases. Conversely, for large horizon areas, these corrections are relatively small and the arealaw is recovered.
Power law corrections to the Bekenstein Hawking entropy has been encountered earlier in other approaches to black hole entropy. For instance, the Noether charge approach predicts a generic power law correction to the BekensteinHawking entropy [11]. For instance, using Noether charge as entropy, it was shown for 5dimensional GaussBonnet gravity
(24) 
that the entropy corresponding to a Killing horizon is [12]
(25) 
Although both these approaches lead to powerlaw corrections, there are couple of crucial differences between the two: (i) In the case of Noether charge, the powerlaw corrections to the BekensteinHawking entropy arises due to the higherderivative terms in the gravity action. However, the corrections we have derived is also valid for EinsteinHilbert action. (ii) The Noether charge entropy does not identify which degrees of freedom contribute most to the entropy. In our case, we have shown that the maximum entropy contribution for the arealaw come close to the horizon while significant contribution to the powerlaw corrections arise from the degrees of freedom far from the horizon [7, 8].
SS is supported by the Marie Curie Incoming International Grant IIF2006039205.
Appendix A Scalar fields in Schwarzschild spacetime
In this section, we generalize the framework of our calculations, so that they are applicable to black hole spacetimes. We start with the Schwarzschild metric with a horizon at :
(26) 
and define the following coordinate transformation from to coordinates:
(27) 
such that (26) transforms to the following metric, in Lemaitre coordinates:
(28) 
The Hamiltonian for a free scalar field in the above spacetime can be
written as
(29) 
Next, choose a fixed Lemaitre time, say and perform the following field redefinitions:
(30) 
Then, at that fixed time, the Hamiltonian (29) transforms to:
(31) 
Note that this is identical to the Hamiltonian in flat spacetime, Eq.(13). Hence, all the analysis in Secs. (2,3) will go through for a blackhole spacetime in a fixed Lemaitre time.
References
Footnotes
 Email: saurya.das@uleth.ca
 Email: Shanki.Subramaniam@port.ac.uk
 Email: sourav.sur@uleth.ca
 the current analysis is done for . For generalization see Ref. [8].
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