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Chaos in black holes surrounded by gravitational waves


Chaos in Black Holes Surrounded by Gravitational Waves
arXiv:gr-qc/9706025v1 10 Jun 1997
P.S. Letelier1 and W. M. Vieira2 Departamento de Matem?tica Aplicada-IMECC a Universidade Estadual de Campinas 13081-970 Campinas, S.P., Brazil
September, 1996

The occurrence of chaos for test particles moving around Schwarzschild black holes perturbed by a special class of gravitational waves is studied in the context of the Melnikov method. The explicit integration of the equations of motion for the homoclinic orbit is used to reduce the application of this method to the study of simple graphics. PACS numbers:04.20.-q, 05.45.+b, 04.20.Jb.

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e-mail: letelier@ime.unicamp.br e-mail: vieira@ime.unicamp.br

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Introduction
There are two main lines of research of chaotic behavior in General

Relativity: one deals with chaoticity associated to inhomogeneous cosmological models, as in Bianchi IX model [1]. The invariance of the relativistic theory challenges the proper concept of chaos in this approach [2]. Although, a gauge invariant method based on Maupertuis principle is proposed in [3] and applied with little changes to the Bianchi IX model [4]. The method points to the occurrence of local instability in this cosmological model near its singularity. This adds to a plethora of early analysis and numerics (see for instance the references cited in [4]), which reinforces the increasingly accepted idea that Bianchi IX is chaotic in some meaningful sense. The other line assumes a given geometry and looks for chaotic behavior of geodesic motion in this background. In this case, the geometry can be taken as either an approximate or an exact solution of Einstein equations. Examples of chaotic geodesic motion are considered in [5] – [8] (exact geometry) and in [9, 10] (approximate). Due to its universality and intrinsic mathematical interest, models in which unstable periodic orbits (UPOs) are subjected to small periodic perturbations has been one of the main paradigms of deterministic chaos [11]. An analytical tool to study these models is the Melnikov function that describes the transversal distance between the unstable and stable manifolds emanating from an UPO. Its isolated odd zeros indicate the crossing of these manifolds, hence the onset of chaos [12, 13]. Examples of applications of the Melnikov method in gravitation are: the gravitational collapse of cosmological models [14], the study of orbits around a black hole perturbed by either gravitational radiation [9] or an external quadrupolar shell [10]. Also for par-

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ticles moving in several models of attractive centers periodically perturbed this method has been applied [15]. In this work we study the occurrence of chaos for test particles moving around a Schwarzschild black hole perturbed by a special class of gravitational waves [16]. Since this perturbation is an exact solution of the ReggeWheeler equations (see for instance [17]) we can study the range of the parameters of the model in order to have chaos. In [9] a similar situation is studied but the perturbations, albeit more general that ours, are known only in the high frequency limit. In the next section we present a summary of the Melnikov method. In Sec. 3 we review the homoclinic orbits for Schwarzschild solution, and present an explicit solution t = t(r) for this orbit. In sections 4 and 5 we consider the perturbations and the the application of the Melnikov method, respectively. In the last section we discuss some of the previous results and also compare our work with the application of the Melnikov method presented in [9].

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The Melnikov method
Let us consider a Hamiltonian, H0 = p2 + V (q), 2m (1)

that admits at least one UPO with the corresponding homoclinic orbit, and also a small periodic perturbation described by the Hamiltonian function ?H1 (q, p, t). Then the transversal distance, in phase space, between the perturbed unstable and the perturbed stable manifolds emanating from the UPO is proportional to [13]


M(t0 ) =
?∞

{H0 , H1 }dt,

(2)

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where the integral is taken along the unperturbed homoclinic orbit, t0 is an arbitrary initial time, and {f, g} = ?f ?g ?g ?f ? , ?p ?q ?q ?p (3)

with (q, p) being canonical conjugated variables. If there is an isolated intersection for some t0 , i.e., an isolated odd zero of M(t0 ), then there will be one for every t0 . This in?nitely many crossings of manifolds will produce a tangle that is the signature of the homoclinic chaos [12, 13]. In particular, if H1 has the form ? H1 (p, q, t) = H1 (p, q) cos(ωt), we have [13]


(4)

M(t0 ) = cos(ωt0 )
?∞

? {H0 , H1 } cos(ωt)dt + sin(ωt0 )

∞ ?∞

? {H0 , H1 } sin(ωt)dt

(5)

Then, in the generic case, we will have isolated zeros when at least one of the integrals of the previous formula is di?erent from zero.

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The homoclinic orbits

We shall consider a relativistic particle moving in a ?x spacetime described by the metric gab . The world-line of a particle will be denoted by xa (s) and its mass by ?. The motion of the particle can be obtained from the action S[x] = ? 2 gab xa xb ds. ˙ ˙ (6)

This action is not reparametrization invariant, but is the simpler for our purposes. s is the proper time along the world-line. The canonical conjugate momentum to xa is pa = ?gab xb and satis?es the mass shell constraint ˙ 4

g ab pa pb = ??2 . The Hamiltonian of the system is H= 1 ab g pa pb . 2? (7)

The background metric will be considered as the metric of a non rotating black hole, i.e., the Schwarzschild metric, ds2 = ?f dT 2 + f ?1 dR2 + R2 (d?2 + sin2 ?d?2 ), (8)

where f = 1 ? 2M/R. Since, T and ? are cyclic variables we have the conserved quantities: dt ds d? . ds (9)

E ≡ ?pT = ?f

L ≡ p? = ?R2 sin2 ?

For planar motion ? = π/2 (p? = p? = 0) we have the equivalent one ˙ dimensional problem of a particle of mass 2?2 moving in the the potential V and constant energy E 2 ? ?2 , ?
2

dR ds

2

+ V (R) = E 2 ? ?2 L2 2ML2 2M?2 + 2? . R R R3 (10)

V (R) = ? U = (2M/L)2 V we ?nd U =? where β = 0 ≤ β ≤ 1/2.

It is convenient to work in dimensionless variables. De?ning r = R/2M and

1 1 (1 ? β 2 ) + 2 ? 3, 3r r r

(11)

have a local maximum (or unstable point, r = ru ) with U(ru ) < 0, we need

1 ? 12M 2 ?2 /L2 < 1. Since U(∞) ? ?O(1/r), in order to

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In Fig.1 we plot U as a function of r = R/2M for various values of β. The unstable periodic orbit (UPO) correspond in phase space to the point equation for the homoclinic orbit, (r, pr ) = (ru , 0). Now by taking U(ru ) = (2M/L)2 (E 2 ??2 ) we get the motion wβ (r ? 1)(r ? ru )(rm ? r) dr =± , dt r 3/2 where rm = 3/(1 ? 2β), and wβ =
3 2

(12)

the constant of motion E to change the parameter of evolution s to the dimensionless time coordinate t = T /2M. So the homoclinic orbit is limited by r = ru and the maximum value r = rm (turning point). This motion equation admits the primitive, ±wβ t = [r(rm ? r)]1/2 /rm + (2 + 2ru + rm ) arctan (rm ? r)/r ? +
5/3 rm /r ? 1 2ru √ arctanh (1 ? ru ) rm ? ru rm /ru ? 1

3(1 ? 2β/(2 ? β)2 . We have used

2 rm ? r √ arctanh . r(rm ? 1) (1 ? ru ) rm ? 1

(13)

We have chosen the constant of integration to have t(r = rm ) = 0. In Fig.2 we show the positive branch of (13) for di?erent values of β. The particle takes an in?nite amount of time to depart (arrive ) from (to) the homoclinic point where the UPO is located, this is a universal behaviour for these type of orbits. The explicit expression (13) for the homoclinic orbit will play an important role in our study of the Melnikov function and its use will be a signi?cant departure from the treatment given in [9] wherein other interesting graphics related with the homoclinic orbit are presented.

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4

The perturbations

The perturbations of the black hole that we shall consider are of the particular class gab + ?hab with gab given by (8) and hT T = ?f XPl cos(σT ) hRR = f ?1 Y Pl cos(σT ) h?? = R2 (ZPl + W Pl ,? ,? ) cos(σT ) h?? = R2 sin2 ?(ZPl + W Pl ,? cot ?) cos(σT ), (14)

where X, Y, Z and W are functions of R to be determined by the Einstein equations Rab (gcd + ?hcd ) = 0. Pl = Pl (cos ?) are the usual Legendre polynomials. When the above mentioned Einstein equations are expanded up to the ?rst order in ? we ?nd a linear system of ?rst order di?erential equations for the functions X, Y, Z and W [17]. The particular separation of the angular part of the perturbation (14) was found by Friedman [18]. Combinations of this variables reduce these equations to the Zerilli equation, i.e., to a Schr¨dinger type of equation with a nontrivial potential [17]. A particular o solution of the ?rst order di?erential equations is X = pq, Y = 3Mq, Z = (R ? 3M)q, W = Rq, where q = f 1/2 /R2 , p = M ? (15)

M 2 + σ 2 R4 . (16) R ? 2M This solution was found by Xanthopoulos [16] using an ad hoc method. We note that it can be easily found in the Zerilli formulation and corresponds to zero Zerilli function Z (+) , Z (+) = 3M R2 ( W ? Y ), nR + 3M R 7 (17)

where n = (l ? 1)(l + 2)/2.

From Eq.(7) we have for the perturbed system (g ab ? ?hab )pa pb = ??2 . (18)

For an even l we have that the perturbations (14) are even functions in the variable cos ?, i.e., we have perturbations with re?ection symmetry with respect the plane ? = π/2. Then, for a particle moving in the plane ? = π/2 these type of perturbations do not change the plane of the orbit. In other words, the perturbation introduces a “perpendicular force” that is an odd function of cos ?. We ?nd for particles moving in the plane ? = π/2, ? pt = H0 + ?H1 , with H1 = ?[ and hT T = ?f pqNl cos(σT ), 3Mq Nl cos(σT ), hRR = f h?? = R2 (R ? 3M)qNl cos(σT ), where Nl is zero for odd l and Nl = (?1)n 1 · 3 · · · (2n ? 1) , (l = 2n). 2 · 4 · · · 2n (22) E 1 3 2 L2 f hT T ? (f pR hRR + 4 h?? )], 2f 2E R (19)

(20)

(21)

The order of Legendre polynomial l enters in a trivial way in this class of planar perturbations, as a multiplication by the constant Nl . The frequency σ not only appears in the oscillating function cos(σT ) but also in p.

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5

The Melnikov function

Now we shall use the fact that we know explicitly the function t = t(r) for the homoclinic orbit to evaluate the Melnikov function. We ?nd M(t0 ) = ? sin(ωt0 )K, with K= J= E Nl J, M
rm ru

(23)

(24) (25)

F (r, β) sin(ωt(r))dr,

where ω = 2Mσ is a dimensionless frequency and F (r, β, ω) = ? ? 1 ? f 2γf 2 1 h?? γf 5 h??,r htt ? htt,r + 5 (f ? ) ? 4 2r 2 2 r 4r (2M)2 2r (2M)2 dr f2 ? + 2 (1 ? 2γf 2 )hrr ? 2r dt The constant γ is de?ned in terms of β as γ =
2

f? 1? h + hrr,r 2 rr r 2

.

(26)

2 (1 27

+ β)(2 ? β)2 , and

1 + 4ωr 4 f 3/2 ? , htt = ? 2 1 ? 2r 2rf 3 ? hrr = 2 1/2 , 2r f ? h?? = f 1/2 (2r ? 3)/2. 2 (2M)

(27)

By t = t(r) in (25) we mean the positive branch of (13). We have used the homoclinic orbit to map the in?nite interval of the integration to a ?nite one. Also, all the quantities appearing in the de?nition of J are dimensionless. Therefore, to have the homoclinic tangle of orbits we need J = 0. The exact computation of J even in the simple case of the perturbations 9

under consideration is hopeless. Nevertheless, the integrand of J is explicitly known in terms of the variable of integration. This fact can be used to study the zeros of J = J(β, ω), or better the range of β and ω in which J = 0, in a simple graphic way. Firstly, it is instructive to plot the function S = sin(ωt(r)) for a ?x β and di?erent values of ω. We ?nd (see Fig.3) that, depending on the value of ω, S does not change sign in a large portion of the interval ru (β) ≤ r ≤ rm (β), e.g., the two bottom curves (from right to left). We also have a very rapid oscillation near the position of the UPO, that is not shown in the graphic. The values of the parameters are ω = 0.15 (top, from right to left), 0.1, and 0.05 (bottom) and β = 1/4. Also it is illuminating to make a graphic of F (r, β, ω) for di?erent values of β and ω in the range of interest ru (β) ≤ r ≤ rm (β). Fig. 4 shows that this function is very well behaved and does not change of sign in the interval of interest. The integrand of J, i.e., F (r, β, ω) sin(ωt(r)) with β = 1/4 and ω=0.1 is presented in Fig.5. The area under the curve is clearly di?erent from zero, then J = 0. In this case the perturbation will originate a chaotic motion of the test particle. The value ω = 0.1 was chosen from the relation ωk ? π/tk , (28)

where tk is the value of the homoclinic orbit that correspond to the maximum value of its curvature k = t′′ /(1 + (t′ )2 )3/2 . For β = 1/4 we have tk =29.3691 and ωk =0.1069. Therefore, we can say that the perturbations with ω < ωk will originate chaotic behaviour.

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6

Discussion

To better understand the particular perturbation (14) we have computed the Kretschmann scalar for the perturbed metric for the particular values of l = 2 and l = 3, we ?nd Rabcd Rabcd = 2M 48M 2 M + ?kl 8 (3M ? R) 1 ? Pl (cos ?), 6 R R R (29)

the numerical constant kl is k2 = 58 and k3 = ?3/2. Thus, we have a the wave has origin in the black hole.

Kretschmann scalar decaying as R?7 for R ? 2M, indicating that part of In this work we have shown that for a particular class of gravitational perturbations we have that the particles moving along timelike geodesics will present a chaotic motion when the frequency of the perturbation is ω < ωk . In the complementary case, ω > ωk our simple graphic method does not apply. But, anyway one can compute numerically the integral J with a great precision ( the integrand is known explicitly). We found that for ω > ωk , J has positive and negative values depending on the values of β. Then for certain speci?c values of β we will have J(β, ω) = 0 and the Melnikov method does not apply to these cases. From the previous analysis it does look like that the generic situation is chaotic, i.e., only for a numerable set of frequencies ω, given a value of β, we should not have chaos. The number of elements of this set increases with ω, but is still numerable. To be more precise, the Melnikov method fails to predict chaos only for a a numerable set of values of the parameters. We note that seldom one can ?nd so easily the parameter range of a given problem that will produce a chaotic situation. Moreover, for parameters outside this range it is reasonable to guess that only for a numerable set of frequencies the integrability is preserved. Therefore, 11

based in our previous analysis, we can conjecture that chaos is generic for the class of perturbed systems studied. In our case, the limit limω→∞ J(β, ω) is not de?ned. Note that in F (β, ω) appears ω 4 and in the integrand we also have cos ωt. In the case analyzed in [9] the perturbation are quite general, but they are known explicitly only in the limit ω → ∞. Their integral essentially, an oscillating function with frequency ω multiplied by another function proportional to ω. Since, in [9], every thing is known only in the limit of in?nite frequency, in order to predict chaotic behaviour, it is necessary to show that their integral is di?erent from zero in the same limit. This point is unclear in the quoted paper. The authors thank CNPq and FAPESP for ?nancial support and Prof. D.V. Gal’tsov (Moscow) for enlightening discussions about black hole perturbations. equivalent to our J has ±∞ integration limits and in the integrand they have,

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References
[1] V.A. Belinskii, I.M. Khalatnikov and E.M. Lifshitz, Adv. Phys. 19, 535 (1970). [2] G. Francisco and G. E. A. Matsas, Gen. Relat. Grav. 20, 1047 (1988). [3] M. Szydlowski, Phys. Lett. A 176, 22 (1993). [4] M. Biesiada, Class. Quantum Grav. 12, 715 (1995). [5] G. Contopoulos, Proc. R. Soc. Lond. A 431, 183 (1990); A 435, 551 (1991). [6] Y. Sota, S. Suzuki and K. Maeda, Class. Quantum Grav. 13, 1241 (1996). See also, W.M. Vieira and P.S. Letelier, Class. Quantum Grav. 13, 3115 (1996). [7] V. Karas and D. Vokrouhlick?, Gen. Rel. Grav. 24, 729 (1992). y [8] W.M. Vieira and P.S. Letelier, Phys. Rev. Lett. 76, 1409 (1996); Errata, 76, 4098 (1996). [9] L. Bombelli and E. Calzetta, Class. Quantum Grav. 9, 2573 (1992). [10] R. Moeckel, Comm. Math. Phys. 15, 415 (1992). [11] V.I. Arnold, “Dynamical systems (Encyclopaedia of mathematical sciences v. III, Springer-Verlag, Berlin, 1988). [12] V.K. Melnikov, Trans. Moscow Math. Soc. 12, 1 (1983) [13] P. Holmes, Phys. Rep. 193, 137 (1990). 13

[14] J. Koiller, J.R.T. de Mello Neto and I. Dami?o Soares, Phys. Lett. 110A, a 260 (1985). [15] P.S. Letelier and W. M. Vieira, “Chaos in periodically perturbed monopole+quadrupole potentials”, Preprint UNICAMP-IMECC/1996. [16] B.C. Xanthopoulos, Proc. Roy. Soc. A 378, 73 (1981). [17] S. Chandrasekhar, “The mathematical theory of black holes”, (Clarendon Press, Oxford, 1983). [18] J.L. Friedman, Proc. Roy. Soc. A 335, 163 (1973).

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FIGURE CAPTIONS

Fig.1. The e?ective U potential is plotted for the dimensionless parameter β = 1/3 (top curve), 1/4, and 1/5 (bottom curve); the maximum value is located at run = 3/(1 + β).

Fig.2. A graphic of the positive branch of Eq. (13) is pictured for values of the parameter β = 1/3 (top curve), 1/4, and 1/5 (bottom curve). We have that the particle takes a ?nite time to travel from rm to the vicinity of run and then takes an in?nite time to arrive to run itself, wherein is located the UPO.

Fig.3. A graphic of S = sin[ωτ (r)] for β = 1/4, and ω =0.05 (bottom curve, from right to left), 0.1, and 0.15 (top curve).

Fig.4. A plot of F (r, β, ω) for β=1/4. Fig.5. A plot of F (r, β, ω) sin(ωt(r)) for β=1/4, and ω= 0.1. We have a rapid oscillation near run (=12/5 ) (not shown in the ?gure), that produce very ?ne spines in the range [-0.03, 0.03].

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