# Axially Symmetric, Asymptotically Flat Vacuum Metric with a Naked Singularity and Closed Timelike Curves

Authors: Debojit Sarma; Faizuddin Ahmed; Mahadev Patgiri
Journal: Advances in High Energy Physics
 (2016)

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## Abstract

We present an axially symmetric, asymptotically flat empty space solution of the Einstein field equations containing a naked singularity. The space-time is regular everywhere except on the symmetry axis where it possesses a true curvature singularity. The space-time is of type D in the Petrov classification scheme and is locally isometric to the metrics of case IV in the Kinnersley classification of type D vacuum metrics. Additionally, the space-time also shows the evolution of closed timelike curves (CTCs) from an initial hypersurface free from CTCs.


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## Body

## 1. Introduction

The weak cosmic censorship hypothesis (WCCH) of Penrose forbids naked singularities to be the end state of gravitational collapse [1, 2]. This statement, although accepted by many, has been neither proved nor disproved and, as a matter of fact, recent studies have shown that naked singularities can be formed in a continual gravitational collapse of a dust cloud beginning from a regular initial data [3], indicating therefore the possibility of naked singularities occurring in nature. Since proving (or disproving) the WCCH has proved to be a difficult task, attempts have been made to provide the theoretical framework to devise a technique to distinguish between black holes and naked singularities from astrophysical data mainly through gravitational lensing. Some significant works in this direction are the study of strong gravitational lensing in the Janis-Newman-Winicour space-time [4, 5] and its rotating generalization [6] and notably (although not an exhaustive list) the work in [7–10]. Other workers have shown that naked singularities and black holes may be differentiated by the properties of the accretion disks that accumulate around them ([11] and references therein). Consequently, the study of naked singularities and space-time with such objects is of considerable current interest.In [11], the authors have enumerated three possible end states of gravitational collapse. Of these, the last one, namely, that matter falls into the space-time singularity preserving its symmetry structure and leading to a final configuration that is vacuum space-time with a singularity that is either naked or covered, is of special interest to us. In this paper, we attempt to construct such space-time—a vacuum solution of Einstein’s equations with a naked singularity. In what follows, we construct a Ricci flat metric with a singularity at r=0, r being the radial coordinate, and show that the space-time is axially symmetric and asymptotically flat. In addition, we find that the metric admits closed timelike curves which appear at a certain moment, implying that it also represents time machine space-time.Closed timelike curves (CTCs), closed timelike geodesics (CTGs), and closed null geodesics (CNGs), which all imply violation of causality, are an intriguing aspect of the general theory of relativity and are present in certain solutions of Einstein’s field equations. Beginning with Gödel’s universe [12], a considerable number of such causality violating solutions have been constructed. van Stockum’s solution [13], found years before Gödel’s, was later shown to possess CTCs [14]. A few other examples of CTC space-time are Bonnor’s rotating dust space-time which has been analysed in [15] and found to have CTCs, Gott’s [16] space-time with two moving cosmic strings and wormhole space-time [17], and a pure radiation metric with CTCs [18]. In fact, over the years, a number of solutions with CTCs have been obtained. CTCs have also been studied in the context of Brans-Dicke gravity [19], where rigid rotation of matter has been shown to generate these closed curves. Ori and coworkers [20–23] have obtained solutions with CTCs which appear after a certain instant, thereby raising the possibility of constructing a workable time machine at least in theory. We place space-time with CTCs (or CTGs or CNGs) into two categories. In the first category, there is the eternal time machine space-time, such as Gödel’s universe where CTCs preexist, while, in the second, there are true time machines where CTCs appear at a certain moment.Solutions with CTGs and CNGs have also been discussed in the literature. Soares found a class of cosmological solutions with rotating dust and electromagnetic fields admitting [24]. Bonnor and Steadman [25] have shown that space-time with two spinning particles, under special circumstances, allows for the existence of CTGs. A class of solutions of Einstein’s field equations with CTGs representing space-time outside a spinning cosmic string surrounded by a region of finite radial extension with vacuum energy and a gas of strings [26] have been recently found. Other examples are cylindrically symmetric space-time [27] which admit CTGs everywhere outside an axis and vacuum space-time with CNGs found quite recently [28].


## 2. Space-Time with a Singularity

Consider the following line element, empty space-time, given by(1)ds2=-sinh2⁡rcosh⁡tcoth⁡tdt2+cosh2rsinh⁡rdr2+csch⁡rdz2+sinh2⁡r22cosh⁡tdtdϕ-sinh⁡tdϕ2.The coordinates are labelled x1=r, x2=ϕ, x3=z, and x4=t and their ranges are r>0, -∞<z<∞, -∞<t<∞ and ϕ is periodic coordinate ϕ~ϕ+ϕ0, with ϕ0>0. The metric is Lorentzian with signature (+,+,+,-) and the determinant of the corresponding metric tensor gμν, det⁡g=-cosh2⁡rsinh4⁡rcosh2⁡t. The metric (1) is a solution of Einstein’s equations in vacuum satisfying the equation Rμν=0.That the space-time represented by (1) is axisymmetric is clear from the following. Consider Killing vector η=∂ϕ having the normal form:(2)ημ=0,1,0,0.The corresponding covector is (3)ημ=sinh2⁡r0,-sinh⁡t,0,2cosh⁡t.The vector (2) satisfies Killing equation ημ;ν+ην;μ=0. Space-time is cyclically symmetric if it admits a Killing vector with spacelike, closed orbits. Axial symmetry means that the space-time contains a nonempty axis of symmetry. The presence of this axis of symmetry is ensured if the norm of ημ vanishes on the axis, that is, at r=0 (see [29, 30] and references therein). In our case, we find that the norm is (4)ημημ=-sinh⁡tsinh2⁡r,which represents spacelike, closed orbits for t<0 and vanishes on the symmetry axis at r→0. The norm of ημ changes sign for t>0 implying the formation of closed timelike curves which are the subject of the next section.The metric has a curvature singularity atr=0. We find that the Kretschmann scalar (1) (5)K=RμνρσRμνρσ=12csch6⁡rand its differential invariant (6)Rμνρσ;λRμνρσ;λ=180csch9⁡rblow up at r=0, indicating a curvature singularity. We also note that both these scalar invariants approach zero rapidly as r increases.The metric (1) belongs to type D in the Petrov classification scheme. To show this, we construct the following set of null tetrads k, l, m, m- for the metric (1). Explicitly, these vectors have the following form: (7)kμ=csch⁡r0,12csch⁡t,0,122+2sech⁡t,lμ=csch⁡r0,-12,0,12-2+2tanh⁡t,mμ=12sinh⁡rsech⁡r,0,isinh⁡r,0,m-μ=12sinh⁡rsech⁡r,0,-isinh⁡r,0,where i=-1. The set of null tetrads above is such that the metric tensor for the line element (1) can be expressed as (8)gμν=-kμlν-lμkν+mμm-ν+m-μmν.The vectors (7) are null vectors and are orthogonal, except for kμlμ=-1 and mμm-μ=1.Using the set of null tetrads above, we find that, of the five Weyl scalars, only(9)Ψ2=Cμνρσkμmνm-ρlσ=12csch3⁡ris nonzero. The metric is clearly of type D in the Petrov classification scheme. It clear from (5), (6), and (9) that these scalars rapidly vanish as r→∞ leading to the conclusion that the metric is asymptotically flat. In fact, all nonzero curvature invariants for the space-time have form Acschn⁡r, A being a real constant and n a positive integer which means that their asymptotic behaviour is the same as that of the scalars in (5), (6), and (9).Vectorkμ is not only null but also geodesic, satisfying kμ;νkν=0. We have calculated the kinematical properties of the metric such as expansion, shear, and twist and they are given by (10)Θ=12k;μμ=0,ω2=12kμ;ν-kν;μkμ;ν=0,σσ-=12kμ;ν+kν;μkμ;ν-Θ2=0.Hence, the space-time admits expansion-free, twist-free, and shear-free null geodesic congruence.Type D vacuum space-time is known and has been classified by Kinnersley [31]. A calculation of the Newman-Penrose spin coefficients [32] shows that, for our case, the spin coefficient ρ=0. Accordingly, the space-time will be placed in case IV of the classification scheme in [31].It is interesting property of the metric (1) that it reduces to the Misner space [33] in two space-time dimensions. To demonstrate this, we first apply transformations t→sinh-1⁡t followed by ϕ→ϕ+2ln⁡t, to get (11)ds2=cosh2⁡rsinh⁡rdr2+csch⁡rdz2+sinh2⁡r-tdϕ2+1tdt2.A further transformation into (11) by (12)ϕ⟶ϕ+ln⁡tyields (13)ds2=cosh2⁡rsinh⁡rdr2+csch⁡rdz2-sinh2r2dtdϕ+tdϕ2.The above reduces to the Misner space for constants r and z, indicating that the metric discussed here is 4D extension of the Misner space.


## 3. CTCs and Cosmic Time Machines

A peculiar property of the space-time (1) is that it generates CTCs at a certain moment exhibiting time machine-like behaviour. Consider closed orbits of constant r=r0>0, z=z0, and t=t0 where r0, z0, and t0 are constants given by 1D line element: (14)ds2=gϕϕdϕ2=-sinh⁡tsinh2⁡rdϕ2.These orbits are null curves at t=t0=0, spacelike throughout t=t0<0, but become timelike; that is, gϕϕ<0 for t=t0>0, which indicates the presence of CTCs. Hence, CTCs form at an instant of time satisfying t=t0>0.That these CTCs evolve from initially spaceliket=constant hypersurface can be determined by calculating the norm of vector ∇μt (or alternately from the value of gtt in inverse metric tensor gμν). A hypersurface t=constant is spacelike when gtt<0, timelike when gtt>0, and null when gtt=0. From the metric given in (1), (15)gtt=sinh⁡tsech2⁡tcsch2⁡r.Thus, a hypersurface t=constant is spacelike for t<0, timelike for t>0, and null at t=0. Thus, the spacelike t=constant<0 hypersurface can be chosen as initial hypersurface over which initial data may be specified. There is a Cauchy horizon at t=0, called chronology horizon, which separates the causal past and future in a past directed and a future directed manner. Hence, the space-time evolves from a partial Cauchy surface (i.e., Cauchy spacelike hypersurface) into a null hypersurface that is causally well-behaved up to a moment, that is, a null hypersurface t=0, and the formation of CTCs takes place from causally well-behaved initial conditions. This type of CTCs is different from those in the Gödel universe [34], where the CTCs preexist, and similar to those in [21], where they form at some moment. The CTCs of the space-time discussed in this paper are analogous to those formed in the Misner space [33]. The metric for the Misner space in 2D is(16)dsMis2=-2dTdX-TdX2,where -∞<T<∞, but the coordinate X is periodic. The curves T=T0, where T0 is a constant, are closed since X is periodic. The curves T<0 are spacelike and T>0 are timelike, while the null curves T=0 form the chronology horizon. The second type of curves, namely, T>0, is closed timelike curves (CTCs).An interesting possible interpretation of the metric (1) is in terms of a cosmic time machine discussed by Clarke and de Felice. They have shown [35] that if continued gravitational collapse leads to a strong curvature singularity, then strong causality is violated. This would mean that the entire space-time becomes causally ill-behaved and a cosmic time machine is the result. They define a cosmic time machine as space-time which is asymptotically flat and admits closed nonspacelike curves [36]. Our space-time may represent such a cosmic time machine.



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*Source: 2546186-2016-11-21.xml*