**Journal of Modern Physics** Vol.4 No.3(2013), Article ID:28854,7 pages DOI:10.4236/jmp.2013.43050

Geometric Aspects of Extremal Kerr Black Hole Entropy

Department of Physics and Astronomy, Macquarie University, Sydney, Australia

Email: katie.howard@mq.edu.au

Received December 30, 2012; revised January 31, 2013; accepted February 11, 2013

**Keywords:** Bifurcate Killing Horizon; Extremal Kerr Black Hole; Black Hole Entropy

ABSTRACT

Extreme Black Holes is an important theoretical laboratory for exploring the nature of entropy. We suggest that this unusual nature of the extremal limit could explain the entropy of extremal Kerr black holes. The time-independence of the extremal black hole, the zero surface gravity, the zero entropy and the absence of a bifurcate Killing horizon are all related properties that define and reduce to one single unique feature of the extremal Kerr spacetime. We suggest the presence of a true geometric discontinuity as the underlying cause of a vanishing entropy.

1. Introduction

One of the most remarkable ideas in black hole theory is the analogy between the laws of classical black hole mechanics and the laws of thermodynamics.

Black hole thermodynamics has become an active area of research since Bekenstein showed that the entropy of a black hole is proportional to the area of the horizon [1]. It is a well known fact now that that a black hole exhibits an unusual similarity to a thermodynamic system.

Our analysis reveals a purely geometrical disparity between the extreme and near extreme Kerr geometries, due to the singular nature of extreme regime. In other words, the approach to extremality is not continuous. The nature of the extremal Kerr metric is very different from other stationary solutions. We focus on relating the entropy of extremal Kerr black holes strictly to their geometric structure. Any classical method involving a finite number of steps used for the extremal case leads to subtle inconsistencies like a vanishing entropy and zero surface gravity while the area of the event horizon still remains positive. Using the near-extremal limit to evaluate the black hole entropy leads to major discontinuities.

Our aim is to understand this discontinuity working solely on pure geometric grounds. The discontinuous nature of entropy during the transition from non-extremal to extremal black hole is directly connected with a discontinuous topological nature of the horizon. The entropy of extremal black holes can’t be determined as a limit of the non-extremal case. The geometry of the extreme black holes could shed some light on understanding black hole entropy in general. Extremal black holes can’t be regarded as limits of non-extremal black holes due to this discontinuity. We suggest that the reason for this discontinuity is that non-extremal and extremal black holes are topologically different and the switch from one to another can’t be done in a continuous manner. In this paper we study various properties of extreme Kerr black holes to expose the underlying topological nature of the discrepancy between extreme and non-extreme regimes.

2. No Evolution or Time Reversibility

It is well known that Einstein’s field equations are timereversal invariant. A maximally extended spacetime includes apart from the black hole solution, its “time-reverse” case. In the non-extreme case, the extended spacetime possesses a bifurcate Killing horizon. In the extreme case (surface gravity), no distinct timereverse equivalent exists, the black hole is time-independent everywhere and possesses a single degenerate Killing horizon. The surface gravity of a black hole can not be reduced to zero within a finite time. In the extended Schwarzschild spacetime, a white hole region becomes the time-reverse of the black hole region. The future event horizon, which separates two regions, is distinct from the past event horizon. The two regions intersect at the bifurcation two-sphere. The time-reverse of one region yields another region. In the non-extremal Kerr extended case, a new region is the time-reverse of the black hole, generating distinct patches in between the two horizons. The extremal Kerr extended spacetime does not contain such a distinct time-reverse patch but always duplicates of the same patch. There is no distinct timereverse region and no distinct event horizon. The extremal Kerr black hole has no time-reverse equivalent or, in other words, it is time-independent everywhere. Furthermore, a naked singularity is composed of one single region and has no time-reverse region, has no event horizon and zero entropy.

In the extremal case, the Killing vector field on the horizon is null on a timelike hypersurface intersecting the horizon and it is spacelike on both sides [2]. The event horizon is determined by a Killing vector field whose causal properties change from timelike to spacelike across the horizon. This Killing horizon becomes null on a timelike hypersurface surrounding the horizon. The presence of a Killing vector field which is timelike in a region around the event horizon is a very peculiar and puzzling feature. The horizon Killing field is spacelike except at the horizon itself [3].

In Boyer-Lindquist coordinates, the Kerr metric is given by

(1)

where

(2)

(3)

(4)

The horizons are situated at, i.e. at,

(5)

The Kerr spacetime gets divided into three regions:

(6)

(7)

(8)

Region I is the exterior, region II lies between the two Killing horizons at, and region III is an asymptotic region. The mass of the black hole is m, its angular momentum, and its event horizon happens at. The extremal case is obtained by setting, in which case there is no region II since the two horizons coincide. The case describes the generic black hole, while describes a naked singularity [4].

The solutions for generate the inner and outer horizons:

.

The metric has two Killing vectors, and. We can construct a Killing vector as a linear combination of two vectors: with being a constant.

Both and are positive but on the ring singularity they vanish.

In the non-extremal case,. is positive for or and zero for and. But is negative in the region representing, always remaining between the horizons. Since any linear combination of the two Killing vectors remains spacelike, is nonstationary.

In contrast, the extreme case has, positive everywhere except at the event horizon where it is zero. If at, we obtain the angular velocity of a zero angular momentum observer (ZAMO). A ZAMO observer exists at every point in the spacetime. The Killing vector is timelike or null. At each point, one can have a different timelike Killing vector (except at the horizon where it vanishes). There is no point where all Killing vectors are spacelike and no region is non-stationary. A general Killing vector field of the generic Kerr solution is given by the linear combination

(9)

where K is a constant. Its norm is

(10)

This can vanish for all only if [5], that is on one of the horizons. It vanishes on the outer horizon if and only if

(11)

The linear combination defines the horizon Killing vector field. We have

(12)

where

(13)

In 3 + 1 decomposition, the Kerr metric becomes:

where

(14)

where we introduced the lapse function N, the shift vector and the induced metric.

Depending on, the solution depicts a black hole or a naked singularity. The lapse function is never negative. Since, and depend only on r and, the lapse function N also depends only on r and and is timeindependent. The induced and the momentum conjugate P^{ab} are time-independent everywhere. Thus, there is no time evolution of the phase space. The coefficients, and can’t be positive and they are independent of time. They all depend on r and: is zero everywhere. is also time-independent and it depends only on r and. The momentum conjugate to, is also time independent. The extrinsic curvature is:

(15)

with the components:

(16)

and

(17)

where

(18)

and

(19)

The momentum conjugate is:

(20)

with the components:

(21)

and

(22)

where

(23)

Obviously is only dependent on r and and consequently it is independent of time. There is only one single classical microstate available.

In the non-extremal case, the region is non-stationary and the general 3 + 1 decomposition in this region has N^{2} positive. However, all components are time dependent. The phase space in is time dependent. The entropy is not vanishing, since there is more than one classical microstate hidden from the outside observer.

3. No Thermality

A non-extremal spacetime with an outer and an inner horizon becomes extremal as the outer horizon approaches the inner one. The two horizons are in equilibrium at two different temperatures and the temerature of the outer horizon approaches zero. Consequently, no thermality is observed at the outer horizon.

In the extremal regime, the flux is the same both outside and inside the horizon and approaches zero on the horizon, with a vanishing temperature in the extremal case. There is a finite discontinuity of flux in the extremal limit of the non-extremal regime. There is no physically acceptable smooth transition from the extremal regime as a limiting case of the non-extremal one and the pure extremal case.

To understand the thermal nature of an extreme black hold, let us firstly find the probability flux across the horizon. To achieve this, we write the Kerr metric in Kruskal coordinates and set for the extreme regime:

(24)

with

(25)

(26)

(27)

The horizon is located at. Introducing the null coordinates with

(28)

(29)

and

(30)

(31)

the surface appears at. The Kruskal coordinates U, V are:

The future horizon is located at:

.

The Killing vector becomes

To find the outgoing probability flux across the horizon, we find:

(32)

We have and . Taking logarithm of both sides we get the flux:

(33)

For any, no thermality is observed. The horizon behaves like a transparent membrane. The flux at, is obtained by regularizing the deltafunction. Using the limit, we obtain:

(34)

The flux when. A finite discontinuity of flux and no thermality is present at the horizon. This discontinuity is not coordinate related. For an extremal black hole, the proper radial distance from the horizon to any point close to the horizon outside or inside, is infinite. It is impossible for any incident particle state to cross the horizon. An extremal black hole cannot absorb or emit particle states. The coordinates, remove the coordinate singularity at the horizon. However fails to be a proper distance. The discontinuity in is not physical. The flux needs an infinite proper time to become zero at the horizon when it is incident either from inside or outside. When equated to the Boltzmann factor, it implies an infinite. This is equivalent to setting a zero temperature for the black hole. In the extremal limit, when [6], the effective temperature is zero and the emission probability is also zero. The flux is the same both outside and inside the horizon and zero at the horizon. This means a vanishing temperature, therefore a finite discontinuity in flux.

4. Vanishing Entropy

An interesting question appears. Where should we calculate the entropy: on (or nearby) the horizon or within the black hole (disc) itself? Is the entropy created immediately after the gravitational collapse, or later during the black hole evolution? The extremal entropy is independent of the black hole evolution and its internal configuretion. Can such a function be purely derived from geometric or topological considerations? The third law of thermodynamics states that the surface gravity vanishing limit cannot be reached within a finite time [7]. Cosmic censorship Conjecture forbids reducing the surface gravity to zero. It is impossible through a finite number of physical processes to reach the zero limit surface gravity. However, the extremal Kerr black hole has a vanishing surface gravity therefore zero temperature.

Statistical mechanics describes the entropy of a system by the natural logarithm of internal states count: S = lnQ. A microstate Q? is a function of the system’s macrostate. The entropy is a function of these variables. An interesting relation between (macroscopic) entropy and statistical thermodynamics (number of microscopic states) becomes evident. Where there is only one microstate, Q = 1 and the entropy is zero, no disorder is present. One single state corresponds to the extremal regime. Extremal black holes can’t be viewed as limits of non-extremal regime because of this discontinuity. Our assessment is that the non-extremal and extremal regimes are topologically different and the discontinuity itself can be explained on geometric grounds.

An infinitesimal perturbation in mass, spin and horizon area can be written in Kerr metric:

(35)

where m and a are the mass and the spin of the black hole.

The horizons form at. The surface gravity is. The Hawking temperature of the black hole is. If we compare it with the first law of thermodynamics,

(36)

and replace the term by, we find that the entropy must be identified with up to an affine constant, which we set to zero by introducing the limit when.

The entropy becomes:

(37)

where is the Bekenstein-Hawking entropy, G is Newton’s constant and A is the event horizon area.

We see that in extremal regime, because. The analogy between the Equations (35) and (36) can’t be done anymore. We also have

(38)

where the right hand side diverges at the limit. The entropy can be now described a function of m with a singularity at the extremal limit.

Let us assume the entropy being an arbitrary function of the area:

(39)

with

(40)

where and are the change in entropy and area of the black hole when the internal configuration is changed (for example, when a particle falls into it). After the particle crosses the horizon, there is no information about its state or status. We therefore assume that it is equally probable for it to exist or not. The minimum entropy change can be written

(41)

where the summation over n represents all possible states of the particle. The proper radius b for an incident particle with mass and center of mass at is

. The minimum change of black hole area can be written

(42)

and, under the non-extremal condition. However, in the extremal limit, the radius b becomes:

(43)

diverging for any. For any small finite, the proper radius of the particle becomes infinite. Therefore we need to have. For (point particle), we have. The change in entropy requires that

(44)

with a discontinuity in the extremal limit.

A semi-classical picture evaluates the gravitational path integral by employing the euclideanized black hole geometry. If we consider the euclideanised case, the metric in n dimensions near the horizon is

(45)

and the proper angle in the plane near the horizon becomes

(46)

where is the N differentiated with respect to r. N depends on the proper angle:

(47)

In two dimensions, the metric near the horizon reduces to:

(48)

with To avoid a conical singularity at the horizon, the period of is identified with, which corresponds to the topology of a disc with zero deficit angle in the plane. This can always be done for non-extremal black holes, as is nonzero. In the extremal case, the proper radius diverges and the proper angle tends to zero. The disk topology is replaced with an annulus one. The topology of the transverse section in either case is. For a wrong periodicity, the geometry would have a singularity at the origin linked to the excess angle, like a cone structure that we may create out of a sheet of paper. The conical excess angle becomes and the topology is that of an annulus. The topology of the transverse section in either case is. An interesting feature of the solution is that the interior of the black hole is completely absent in the euclidean case. To know what is happening inside the black hole, the euclideanized spacetime is continued to an imaginary value of the radial coordinate near the horizon.

The Euclidean action leads to the entropy

(49)

The euclideanized version imposes in the metric, with leading to a manifold topology. The polar coordinates are defined on the with origin and periodicity of the Euclidean time angle. An interesting fact is that the Lorentzian manifold regions can’t be included in the Euclidean solution. The boundary contributions from the vicinity of the origin for the non-extremal regime are independent of and the canonical action is proportional to, leading to Bekenstein-Hawking entropy [8]. The contribution does not degenerate at the origin because.

In the extremal regime, is infinitely far away from any point outside the horizon and consequently this point must be removed from the whole Euclidean manifold. The extremal black hole horizon is an infinite proper distance from any stationary observer. There is an absence of a conical singularity at the origin of the manifold. The topology of the Euclidean extremal solution becomes. The periodicity of the the Euclidean time is not fixed. Because the origin doesn’t exist any more, for any periodicity of the Euclidean time, no conical singularity is formed [9]. The origin is not part of the manifold and the contribution from the vicinity of the origin vanishes. Consequently the entropy is zero.

We believe that this topology can explain what is actually happening with the entropy. If we consider the black hole as a microcanonical ensemble, in a Hamiltonian formulation, the action I is proportional to the entropy. A dimensional continuation of Gauss-Bonnet theorem to n dimensions gives us the action:

(50)

with the Euler characteristic of the euclideanised plane and the area of the transverse. The black hole entropy becomes

(51)

In the non-extremal regime, corresponding to a disc and leading to the regular area law. In the extremal case, we have (annulus), implying a vanishing entropy.

5. Discussion

Cosmic Censorship tries to solve the following problem: can a singularity exist in the absence of a horizon (naked singularity, not a topic of this paper)? Similarly, the existence of extreme black holes relies upon answering the question: can a spinning singularity exist without two separate horizons? This is an interesting problem. Extremal Kerr black holes are stationary black holes whose inner and outer horizons coincide. An extremal black hole has and no bifurcate Killing horizon. Also, the past and future horizons never intersect. There is no physical process that can make an extremal black hole out of a non-extremal black hole. A near-extremal black hole has a sort of potential barrier close to the horizon that prevents to reach extremal regime. These type of black holes represent the asymptotic limit of physical black holes [10]. Extremal black holes never behave as thermal objects. Their temperature is always undefined and their emission spectrum is non-planckian. Their nonthermal nature is a consequence of the geometric nature of the horizon. All characteristics of the stress-energy tensor are different from those in the non-extremal regime. A final thermal macrostate can’t be achieved in a smooth continuous way without violating the energy conditions. The extremal Kerr black hole cannot be produced through a process involving any finite number of steps without violating the weak energy condition. Consequently an extremal black hole cannot be produced through a finite number of processes or through standard gravitational collapse.

However, black hole entropy can be also defined as a measure of the observer’s accessibility to information about the internal configuration hidden behind the event horizon. This internal configuration can be depicted as the sum of points in the phase space, defined by a number of classical microstates. We can say that extremal Kerr black hole has zero entropy because it possesses a single classical microstate. Extremal black holes have zero temperature, surface gravity and zero entropy therefore they obey the strong version of the third law of thermodynamics.

We could say that an extremal Kerr black hole has zero entropy only because it has one single classical microstate. There is no continuous set of classical states and no time evolution. All metric components are time independent. Any observer should have complete access to the unique classical state found within the region beyond the event horizon.

A regular black hole has non-zero entropy because an event horizon hides its internal configuration and there are more than one internal states within its configuration. An extremal black hole has an event horizon but because the phase space is time independent, it doesn’t hide more than one internal configuration. The extremal solution doesn’t have a time-reverse equivalent or a bifurcate Killing horizon. The condition for a non-zero entropy is the existence of a bifurcate Killing horizon in the extended spacetime. Wald’s general formula for the entropy of a black hole [11] should be calculated at the bifurcation two-sphere not on the event horizon. The entropy is calculated as the integral of a geometric quantity over the spacelike cross section of the event horizon. The generated entropy at the event horizon represents the Noether charge of the Killing isometry that generates the event horizon itself. This geometric origin of the entropy suggest a deeper connection between the gravitational entropy, the topological structure of the spacetime and the nature of gravity. We suggest a purely local and geometrical character of the entropy. The different nature of the event horizon in the regular and extreme case requires different calculations of the entropy. The thermodynamic features are consequences of the topological structure of the space-time. The geometric nature of the boundary of the manifold determines the character of the entropy of the black hole. In the non-extremal regime, the proper distance and the coordinate distance between the inner and outer horizons are finite. In the extremal case, the proper distance between the event and Cauchy horizons becomes infinite, even though the coordinate distance vanishes. All these peculiar features are connected to a major property of extremal geometry: the absence of outer trapped surfaces within the horizon, which will be the subject of further work. Wald also assumed a local, geometrical character of the concept of black hole entropy [12], when he calculated the entropy at the bifurcation two-sphere. Entropy is depicted as a local geometrical quantity integrated over a spacelike region of the horizon.

For a regular black hole, the zeroth law imposes that the horizon of a black hole must be bifurcate and the surface gravity must be must constant and non-vanishing. In the case of a degenerate Killing horizon there is no such bifurcation between the horizons. The area between horizons is completely absent.

6. Conclusion

The primary condition for a non-zero entropy is the existence of a bifurcate Killing horizon. This single criteria is enough. We analyzed a few features of the Kerr black hole that distinguish the extremal regime from the nearextremal one. From a thermodynamic point of view, there is a discontinuous nature of the entropy between the non-extremal and extremal cases, as the entropy of extremal regime is not the limit of the non-extremal one. While dual and string theory dual microstate counting predict non-vanishing entropy solutions for extreme regime, we suggested that the unusual nature encountered in the extremal limit using semi-classical methods represents a genuine relevant topological discontinuity and therefore the origin of a vanishing entropy. The entropy is zero, in agreement with semi-classical solutions, due to a degeneracy of the horizon geometry. The spacetime topology plays an essential role in the explanation of intrinsic thermodynamics of the extreme black hole solution. We conclude that the topology itself of the extreme black hole is enough to explain entropy in this regime. Moreover, the study of extreme black holes could play a crucial role in understanding gravitational entropy in general.

REFERENCES

- J. D. Bekenstein, “Black Holes and Entropy,” Physical Review D, Vol. 7, No. 8, 1973, pp. 2333-2346. doi:10.1103/PhysRevD.7.2333
- S. W. Hawking and G. F. R. Ellis, “The Large Scale Structure of Space-Time,” Cambridge University Press, Cambridge, 1973.
- B. O’Neill, “The Geometry of Kerr Black Holes,” A K Peters, Wellesley, Massachusetts, 1995.
- S. Chandrashekar, “The Mathematical Theory of Black Holes,” Clarendon Press, Oxford, 1983.
- C. W. Misner, K. S. Thorne and J. A. Wheeler, “Gravitation,” W. H. Freeman, San Francisco, 1973.
- R. Geroch, “Limits of Spacetimes,” Communications in Mathematical Physics, Vol. 13, No. 3, 1969, pp. 180-193. doi:10.1007/BF01645486
- I. Racz, “Does the Third Law of Black Hole Thermodynamics Really Have a Serious Failure?” Classical and Quantum Gravity, Vol. 17, No. 20, 2000, pp. 4353-4356. doi:10.1088/0264-9381/17/20/410
- S. W. Hawking, et al., “Entropy, Area, and Black Hole Pairs,” Physical Review D, Vol. 51, No. 8, 1995, pp. 4302-4314. doi:10.1103/PhysRevD.51.4302
- J. Bardeen and G. T. Horowitz, “The Extreme Kerr Throat Geometry: A Vacuum Analog of AdS2 S2,” Physical Review D, Vol. 60, No. 10, 1999, Article ID: 104030. doi:10.1103/PhysRevD.60.104030
- A. J. Amsel, G. T. Horowitz, D. Marolf and M. M. Roberts, “No Dynamics in the Extremal Kerr Throat,” Journal of High Energy Physics, Vol. 2009, 2009, p. 044. doi:10.1088/1126-6708/2009/09/044
- R. M. Wald, “General Relativity,” The University of Chicago Press, Chicago, 1984.
- R. M. Wald, “Black Hole Entropy Is the Noether Charge,” Physical Review D, Vol. D48, No. 8, 1993, pp. 3427- 3431. doi:10.1103/PhysRevD.48.R3427