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On vacuum gravitational collapse in nine dimensions

P. Bizo? ,1 T. Chmaj,2, 3 A. Rostworowski,1 B. G. Schmidt,4 and Z. Tabor5 n

2 1 M. Smoluchowski Insitute of Physics, Jagiellonian University, Krak?w, Poland o H. Niewodnicza?ski Institute of Nuclear Physics, Polish Academy of Sciences, Krak?w, Poland n o 3 Cracow University of Technology, Krak?w, Poland o 4 Max-Planck-Institut f¨r Gravitationsphysik, Albert-Einstein-Institut, Golm, Germany u 5 Department of Biophysics, Jagellonian University, Krak?w, Poland o (Dated: February 4, 2008)

We consider the vacuum gravitational collapse for cohomogeneity-two solutions of the nine dimensional Einstein equations. Using combined numerical and analytical methods we give evidence that within this model the Schwarzschild-Tangherlini black hole is asymptotically stable. In addition, we brie?y discuss the critical behavior at the threshold of black hole formation.

arXiv:gr-qc/0511064v1 12 Nov 2005

Introduction and setup: Over the past few years there has been a surge of interest in higher dimensional gravity, motivated by several reasons. The main reason comes from the new brane-world scenario in string theory according to which we live on a three dimensional surface (called a brane) in a higher dimensional spacetime [1]. In order to understand the phenomenology of this scenario and its experimental predictions, like production of black holes in the next generation of colliders, it becomes important to study solutions of Einstein’s equations in more than four dimensions. Another reason, closer to our own motivation, has nothing to do with string theory and comes from general relativity itself. Viewing the dimension of a spacetime as a parameter of the theory is helpful in understanding which features of general relativity depend crucially on our world being four dimensional and which ones hold in general. Last, but not least, extra dimensions are fun. In a recent paper [2] some of us showed that in ?ve spacetime dimensions one can perform a consistent cohomogeneity-two symmetry reduction of the vacuum Einstein equations which – in contrast to the spherically symmetric reduction – admits time dependent asymptotically ?at solutions. The key idea was to modify the standard spherically symmetric ansatz by replacing the round metric on the three-sphere with the homogeneously squashed metric, thereby breaking the SO(4) isometry to SO(3) × U (1). In this way the squashing parameter becomes a dynamical degree of freedom and the Birkho? theorem is evaded. This model provides a simple theoretical setting for studying the dynamics of gravitational collapse in vacuum, both numerically [2] and analytically [3]. As mentioned in [2], similar models can be formulated in higher D = n + 2 dimensions as long as the corresponding sphere S n admits a non-round homogeneous metric, i. e. there exists a proper subgroup of the orthogonal group SO(n + 1) which acts transitively on S n . According to the classi?cation given by Besse [4], such transitive actions exist on all odd dimensional spheres. For example, the group SU (n + 1) acts transitively on S 2n+1 and the group Sp(n + 1) acts transitively on S 4n+3 . It is natural to ask whether the properties of gravitational collapse found in [2] are typical for this class of models or whether new phenomena appear in higher dimensions. A systematic analysis of this question appears hopeless in view of the fact that the number of degrees of freedom (squashing parameters) grows quickly with dimension, thus it seems useful to look at speci?c examples to get better understanding. In this note we consider a model with one degree of freedom which describes the squashing of the seven sphere. More concretely, we regard S 7 as the coset manifold Sp(2)/Sp(1) ? SO(5)/SO(3), or equivalently, as the S 3 bundle over the S 4 base space with SO(5) × SO(3) invariant metric. In the past, such the squashed seven sphere has attracted a great deal of attention in the context of eleven dimensional supergravity [5]. We parametrize the metric in the following way ds2 = ?Ae?2δ dt2 + A?1 dr2 + r2 d?2 , 7 where d?2 7 is the metric on the unit squashed S [6] d?2 = 7 B, A, and δ are functions of t and r, ei = 1 sin ? (σi ? σi ), ? 2 Ei = cos2 ? ? σi + sin2 σi , ? 2 2 σ3 = dψ + cos θdφ, (3) 1 3B 1 2 e (d?2 + e2 ) + e?4B Ei , i 4 4 (2)

7

(1)

and σi and σi are two sets of left-invariant one-forms on SU (2) ? σ1 = cos ψdθ + sin ψ sin θdφ, σ2 = ? sin ψdθ + cos ψ sin θdφ, (4) ? ? ? with σi given by identical expressions in terms of (ψ, θ, φ). In this ansatz the SO(8) isometry of the round S 7 is ? broken to SO(5) × SU (2). This is a special case of a more general ansatz for which the S 3 ?bers are allowed to be squashed themselves [7].

2 Substituting the ansatz (1) into the vacuum Einstein equations, Rαβ = 0, we get equations of motion for the functions A(t, r), δ(t, r) and B(t, r) (in the following we use overdots and primes to denote ?t and ?r , respectively) A′ = ? 6A 1 2 ˙ 48e?3B ? 12e?10B + 6e4B ? 3r e2δ A?1 B 2 + AB ′ + r 7r ˙ ˙ A = ?6rABB ′ ,

′ 2δ ?2

(5) (6) (7)

δ = ?3r e A ˙ eδ A?1 r7 B

·

˙ B 2 + B ′2 ,

′

? e?δ Ar7 B ′

4 + e?δ r5 6e?3B ? e4B ? 5e?10B = 0. 7

(8)

It follows immediately from the above equations that if B = 0 (no squashing), then δ = 0 and either A = 1 6 (Minkowski), or A = 1 ? rh /r6 (Schwarzschild-Tangherlini), where rh is the radius of the black hole horizon. We showed in [2] that the analogous two solutions in ?ve dimensions play the role of generic attractors in the evolution of regular asymptotically ?at initial data (small and large ones, respectively) and the transition between these two outcomes of evolution exhibits the type II discretely self-similar critical behavior. The aim of this note is to show that these properties are also present in nine dimensions which suggests that they are general features of vacuum gravitational collapse for this class of models. Linear stability and quasinormal modes: Before presenting numerical evidence for the nonlinear stability of the Schwarzschild-Tangherlini solution, we want to discuss the results of linear perturbation theory. Linearizing equations (5)-(8) around the Schwarzschild-Tangherlini solution we obtain the linear wave equation for the perturbation δB(t, r) 1 16A0 ¨ δB ? 7 A0 (r7 A0 δB ′ )′ + 2 δB = 0, r r A0 = 1 ? 1 , r6 (9)

where we have used the scaling freedom to set the radius of the horizon rh = 1. Introducing the tortoise coordinate x de?ned by dx/dr = A?1 , and substituting δB(t, r) = e?ikt r?7/2 u(x) into (9) we get the Schr¨dinger equation on o 0 the real line ?∞ < x < ∞ ? d2 u + V (r(x))u = k 2 u, dx2 V (r) = 1 4 1? 1 r6 99 49 + 8 r2 r . (10)

This equation is a special case (corresponding to the gravitational tensor perturbation with l = 2) of the master equation for general perturbations of the higher dimensional Schwarzschild-Tangherlini solutions derived independently by Gibbons and Hartnoll [8] and Ishibashi and Kodama [9]. Since the potential in (10) is everywhere positive, there are no bound states, which implies that the Schwarzschild-Tangherlini black hole is linearly stable. We computed quasinormal modes, i.e. solutions of equation (10) satisfying the outgoing wave boundary conditions u ? e±ikx for x → ±∞, using Leaver’s method of continued fractions [10, 11]. Substituting u(x(r)) = r?1 r+1

?ik/6 ∞

eikr

n=0

an

r?1 r

n

,

a0 = 1,

(11)

into (10) we get a 12-term recurrence relation for the coe?cients an . The prefactor in (11) ful?lls the outgoing wave boundary conditions both at the horizon and at in?nity, hence the quasinormal frequencies are given by the discrete values of k for which the series in (11) converges at r = ∞. Using Gaussian elimination [11] we reduced the 12-term ∞ recurrence relation to a 3-term one. According to Leaver [10], the convergence of the series n=0 an is equivalent to a condition under which the 3-term recurrence relation has a minimal solution. Such the condition, formulated in terms of continued fractions, yields the transcendental eigenvalue equation which has to be solved numerically. The full details of this computation will be described elsewhere. Here, in order to interpret numerical results we need only ?1 to know that the fundamental quasinormal mode has the frequency k0 = 3.4488 ? 0.8601i (in units rh ). This mode is expected to dominate the process of ringdown. The higher modes are damped much faster (for example, the ?rst overtone has the frequency k1 = 2.7548 ? 2.6116i) so in practice they play no role in the dynamics. Numerical results: Using the same ?nite-di?erence code as in [2] we solved equations (5)-(8) numerically for several families of regular initial data. We found that the overall picture of dynamics of gravitational collapse looks qualitatively the same as in ?ve dimensions, that is, we have dispersion to the Minkowski spacetime for small data and collapse to the Schwarzschild-Tangherlini black hole for large data (see Fig. 1a). In the latter case we looked in more detail at the asymptotics of this process. We found that at some intermediate times the solution settling down to the Schwarzschild-Tangherlini black hole is well approximated outside the horizon by the least damped quasinormal mode. This is shown in Fig. 1b.

3

0.6 t=0 t=5 t=7 t=9 t=11 t=13 t=15

0

0.5

-5

numerical solution fundamental QNM

0.4

-10

0.3

ln|B(t,5)|

4 6 8 10

m(t,r)

-15

0.2

-20

0.1

-25

0 0 2

-30 6 8 10 12 14 16 18 20

r

t

(a)

Formation of a black hole

(b)

Quasinormal ringing

FIG. 1: (a) For a black-hole solution we plot a series of late-time snapshots of the mass function m(t, r). The initial mass function (solid line) has the form of a kink asymptoting the total mass m(∞) = 0.575. During the evolution the horizon 6 develops at rh = 0.606 which corresponds to the black hole mass mBH = rh = 0.05. Thus, only a small fraction of the total mass gets trapped inside the horizon while the remaining mass is being radiated away to spatial in?nity, as is clearly seen from the plot. (b) We plot the time series ln |B(t, r0 )| at r0 = 5 for the same solution as in (a), and superimpose the fundamental quasinormal mode with frequency k0 = (3.4488 ? 0.8601 i)/rh . On the time interval 10 < t < 16 we get very good agreement between these two curves which con?rms a well-known fact that quasinormal modes encode an intermediate time behavior of solutions at a ?xed point in space [12].

-15 0.14 0.12 0.1 0.08 ? ~ 0.78 B(ln(r),T0) B(ln(r)+?,T1) B(ln(r)+2?,T2) B(ln(r)+3?,T3) -20 -25 γ ~ 1.64

ln(mBH)

B(t,r)

-30 -35 -40 -45 -50 -30 numerical data linear fit

0.06 0.04 0.02 0 -0.02 -0.04 -8 -7 -6 -5 -4 -3 -2 -1 0

-25

-20

-15

-10

ln(r)

ln(p-p*)

(a)

Discrete self-similarity

(b)

Black-hole mass scaling

FIG. 2: (a) For a near-critical evolution we plot the function B at some late central proper time T0 and superimpose the next three echoes (at times Tn ) shifted by ln(r) → ln(r) + n?. Minimization of the discrepancy between the pro?les yields ? ≈ 0.78. (b) For supercritical solutions the logarithm of black hole mass mBH is plotted versus the logarithmic distance to criticality. A ?t of the power law ln(mBH ) = γ ln(p ? p? ) + const yields γ ≈ 1.64. The small wiggles around the linear ?t are the imprints of discrete self-similarity; their period is equal to 2.87 in agreement with the theoretical prediction 6?/γ.

At the threshold for black hole formation we observe the type II discretely self-similar critical behavior with the echoing period ? ≈ 0.78 and the black-hole mass scaling law with the universal exponent γ ≈ 1.64. This is shown in Fig. 2. Note that in eight space dimensions, mass has the dimension of length6, hence γ = 6/λ, where λ is the eigenvalue of the growing mode of the critical solution. Strangely enough, the product ?λ ≈ 2.85 is approximately the same (up to numerical errors) as in ?ve dimensions [2]. We do not know whether there is any deeper meaning behind this numerical coincidence.

4 Final remarks: In this note we have focused on similarities between the models in ?ve and nine dimensions, however at the end we would like to mention two interesting qualitative di?erences which in our opinion are worth investigation. The ?rst di?erence is the existence of the second static solution corresponding to the non-round homogeneous Einstein metric on S 7 B= ln 5 , 7 A = 9 · 5?10/7 1 ?

6 rh r6

,

δ = 0.

(12)

This solution is asymptotically conical so it does not participate in the dynamics of asymptotically ?at initial data. It would be interesting to study the evolution of non-asymptotically ?at initial data and determine a dynamical role of the solution (12), as well as other known explicit solutions, like for example the Spin(7) solution [13]. The second di?erence is the lack of monotonicity of the mass function m(t, r), de?ned by A = 1 ? m(t, r)/r6 . From the hamiltonian constraint (5) we obtain ˙ m′ = 3r7 e2δ A?1 B 2 + AB ′

2

1 + r5 42 ? 48e?3B + 12e?10B ? 6e4B . 7

(13)

The potential term on the right hand side of this equation has the local minimum equal to zero at B = 0, the local maximum at B = ln 5/7, and is negative for large positive values of B. Thus, the mass density may be locally negative and, indeed, it is easy to construct initial data with large regions of negative mass density. This suggests a possibility of violating the weak cosmic censorship (note that monotonicity of mass is essential in the Dafermos and Holzegel proof [3]). Although our preliminary numerical attempts failed to produce a counterexample, i.e. a generic naked singularity, this problem deserves more systematic investigation. We should stress that despite locally negative mass density the total mass m(∞) is guaranteed to be nonnegative by the positive mass theorem in higher dimensions [14]. It would be interesting to prove this fact in our model in an elementary manner. In particular, for time-symmetric initial data it follows from equation (13) and the requirement of regularity at the origin, m(0) = 0, that m(∞) = e

?

∞ 0

3rB ′2 dr 0

∞

r

e

0

3ρB ′2 dρ

1 2 3r7 B ′ + r5 (42 ? 48e?3B + 12e?10B ? 6e4B ) dr. 7

(14)

We challenge the readers to show that this integral is nonnegative for all ”reasonable” functions B(r) which vanish at the origin and have compact support (or fall o? faster than r?3 at in?nity). Finally, we remark that there is 6 an analogous problem for the black-hole boundary condition, m(rh ) = rh , where one wants to prove the Penrose inequality m(∞) ≥ m(rh ). Acknowledgments: PB is grateful to Gary Gibbons for discussions, remarks and sharing his notes. PB acknowledges the hospitality of the Isaac Newton Institute in Cambridge where this work was initiated. This research was supported in part by the Polish Ministry of Science grant no. 1PO3B01229.

[1] [2] [3] [4] [5] [6] [7] [8] [9] [10] [11] [12] [13] [14]

L. Randall and R. Sundrum, Phys. Rev. Lett. 83, 4690 (1999). P. Bizo?, T. Chmaj, and B. G. Schmidt, Phys. Rev. Lett. 95, 071102 (2005). n M. Dafermos and G. Holzegel, gr-qc/0510051 A. L. Besse, Einstein Manifolds (Springer, New York, 1987). M. J. Du?, B. E. W. Nilsson, and C. N. Pope, Phys. Rev. Lett. 50, 2043 (1983). M. A. Awada, M. J. Du?, and C. N. Pope, Phys. Rev. Lett. 50, 294 (1983). M. Cvetic, G. W. Gibbons, H. Lu, and C. N. Pope, Nucl. Phys. B620, 29 (2002). G. Gibbons and S. A. Hartnoll, Phys. Rev. D66, 064024 (2002). A. Ishibashi and H. Kodama, Prog.Theor.Phys. 110, 901 (2003). E.W. Leaver, Proc. Roy. Soc. Lond. A402, 285 (1985). E.W. Leaver, Phys. Rev. D41, 2986 (1990). K. D. Kokkotas and B. G. Schmidt, Living Rev.Rel. 2, 2 (1999). G. W. Gibbons, D. N. Page, and C. N. Pope, Comm. Math. Phys. 127, 529 (1990). J. Lohkamp, Math. Ann. 313, 385 (1999).

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