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Alignment of Quasar Polarizations on Large Scales Explained by Warped Cosmic Strings

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Received 21 February 2016; accepted 22 March 2016; published 25 March 2016

1. Introduction

Physicists speculate that extra spatial dimensions could exist in addition to our ordinary 4-dimensional spacetime. The underlying theory is the string theory, an unified description of gauge interactions and gravity. String theory could provide an adequate description of quantum gravity and can be used to explain the several shortcomings of the Standard Model and modern cosmology, i.e., the unknown origin of dark energy and dark matter, the weakness of gravity ( hierarchy problem) and the incredibly fine-tuning of the cosmological constant. Moreover, the recently found evidence for the acceleration of our universe could be explained in these so-called super-string models without the need for a cosmological constant (self-acceleration). However, its weak point is, that it is extremely hard to make predictions which are testable at energies available in experiments because the theory will manifest itself at energies of the order of the fundamental Planck scale, dependent of the number of the extra dimensions. The observed 4-dimensional Planck scale is given by Newton’s constant and is. String theory also predicts the existence of sub-manifolds of the “bulk” spacetime, the so-called branes: it may be that our (3 + 1)-dimensional spacetime is such a 3-brane. All standard model fields resides on the brane, while gravity can propagate into the bulk. The fundamental scale in elementary particle physics, the electroweak scale, is of order. In order to lower down the fundamental scale of super string theory to the electroweak scale, one conjectures that the 4-dimensional Planck scale is not fundamental, but only an effective scale which can become much larger than the if the extra dimensions L

are much larger than [1] . For, the fundamental Planck scale can be of the order of the

electroweak scale. Within this brane world picture, at low energies, gravity is localized at the brane and general relativity is recovered, but at high energy gravity “leaks” into the bulk. Recently there is growing interest in the warped brane world model [2] , where there is one preferred extra dimension, with other extra dimensions treated as ignorable. The extra dimension is curved (or warped) rather than flat. This means that self-gravity of the brane is incorporated.

It is conjectured that one needs an inflaton field in the very early stages of our universe to solve the problems in the standard model of cosmology, i.e., the horizon and flatness problem. The inflationary cold dark matter model with a cosmological constant (LCDM) could be a good candidate if one abandons the cosmological constant problems. It can explain the fluctuations we observe in the cosmic microwave background (CMB). The inflaton field could be the well-known scalar-Higgs field. This field has lived up to its reputation. It originates from the theory of type II superconductivity, where vortex lines occur as topological defects in an abelian U(1) gauge model, which is coupled to a charged scalar field. It explains the famous Meissner effect (Ginzburg- Landau theory). Topological defects can occur when the field symmetries are broken. In cosmology, this happens when the universe cools down [3] . Topological defects, such as cosmic strings, monopoles and textures, can have cosmological implications. Apart from their possible astrophysical roles, topological defects are fascinating objects in their own right and can give rise to a rich variety of unusual phenomena. The U(1) vortex solution possesses mass, so it will couple to gravity. It came as a big surprise that there exists vortex-like solutions in general relativity. It is conjectured that any field theory which admits cosmic string solutions, a network of strings inevitable forms at some point during the early universe. However, it is doubtful if they will persist to the present time in the LCMD model. Evidence of these objects would give us information at very high energies in the early stages of the universe. It is believed that the grand unification (GUT) energy scale of symmetry breaking is about. The thickness of a cosmic string is and the length could be unbounded long. The mass per unit length of a cosmic sting will be of the order of 10^{18} kg per cm, which is proportional to the square of the energy breaking scale. The thickness is still a point of discussion. By treating the cosmic string as an infinite thin mass distribution, one will encounter serious problems in general relativity. This infinite thin string model give rise to the “scaling solution”, i.e., a scale-invariant spectrum of density fluctuations, which in turn leads to a scale invariant distribution of galaxies and clusters. It was believed that cosmic strings could have served as seeds for the formation of galaxies. Cosmic strings can collide with each other and will intercommute to form loops. These loops will oscillate and loose energy via gravitational radiation and decay. There are already tight constraints on the gravitational wave signatures due to string loops via observations of the millisecond pulsar-timing data, the cosmic background radiation (CMB) by LISA and analysis of data of the LIGO-Virgo gravitational-wave detector. Its spectrum will depend on the string mass, where is the mass per unit length. Recent observations from the COBE, Wamp and Planck satellites put the value of. It turns out that cosmic strings can not provide a satisfactory explanation for the magnitude of the initial density perturbations from which galaxies and clusters grew. The interest in cosmic strings faded away, mainly because of the inconsistencies with the power spectrum of the CMB. Moreover, they will produce a very special pattern of lensing effect, not found yet by observations. New interest in cosmic strings arises when it was realized that cosmic strings could be produced within the framework of string theory inspired cosmological models. Investigations on cosmic strings in warped brane world models show consistency with the observational bounds [4] [5] . The warp factor makes these strings consistent with the predicted mass per unit length on the brane, while brane fluctuations can be formed dynamically due to the modified energy- momentum tensor components of the scalar-gauge field. This effect is triggered by the time-dependent warp factor. The recently discovered “spooky” alignment of quasar polarization over a very large scale [6] could be well understood by the features of the cosmic strings in brane world models and could be the first evidence of the existence of these strings.

In Section 2 we will outline the warped 5-dimensional model. In Section 3 we apply the multiple-scale approximation in order to find an wavelike solution to first order of the Einstein and matter field equations.

2. The Warped 5D Model

Let us consider the warped five-dimensional Friedmann-Lematre-Robertson-Walker (FLRW) model in cylin- drical polar coordinates

(1)

The function is the warp factor and y the extra (bulk) dimension. Here and are functions of, while is a function of. Our 4-dimensional brane is located at. All standard model

fields reside on the brane, while gravity can propagate into the bulk. We consider a scalar-gauge field on the brane in the form [7]

(2)

with the vacuum expectation value of the scalar field and the coupling constant. As potential we take the well-known “mexican hat” potential. From the Einstein equations on the 5-dimensional spacetime one obtains a solution for the warp factor [5]

(3)

with and some constants and the bulk cosmological constant. The first term in Equation (3) is just the warp factor of the Randall-Sundrum model. The second term modifies the effective 4D Einstein equations. The Einstein field equations induced on the brane can be derived using the Gauss-Codazzi equations and the Israel-Darmois junction conditions. The modified Einstein equations become [8]

(4)

with the Einstein tensor calculated on the brane metric and the unit vector normal to the brane. In Equation (4) the effective cosmological constant

and is the vacuum energy in the brane (brane tension). The latter equality sign is a consequence of the

relation between the 4- and 5-dimensional Planck mass in the braneworld approach,. If in addition the brane tension is related to the 5-dimensional coupling constant and the cosmological constant by, then and we are dealing with the RS-fine tuning condition [2] . The first correction term in

Equation (4) is the quadratic term in the energy-momentum tensor arising from the extrinsic curvature terms in the projected Einstein tensor

(5)

The second correction term in Equation (4) is given by

(6)

and is a part of the 5D Weyl tensor and carries information of the gravitational field outside the brane and is constrained by the motion of the matter on the brane, i.e., the Codazzi equation. The scalar-gauge field equation becomes [7]

(7)

with, the covariant derivative with respect to, the gauge coupling constant and the star represents the complex conjugated. is the Maxwell tensor.

From Equation (4) together with the matter field equations Equation (7), one obtains a set of partial differential equations, which can be solved numerically [5] . Because gravity can propagate in the bulk, the cosmic string can build up a huge mass per unit length (or angle deficit) by the warp factor and can induce massive KK-modes felt on the brane, while the manifestation in the brane will be warped down to GUT scale, consistent with observations. Disturbances in the spatial components of the stress-energy tensor cause cylindrical symmetric waves, amplified due to the presence of the bulk space and warp factor. They could survive the natural damping due to the expansion of the universe. These disturbances could have a profound influence on the expansion of the universe. There could even be a “self-acceleration” without the need of an effective brane cosmological constant [9] .

Besides the numerical solutions of the field equations, one should like to find an approximate wave solution where one can recognize the nonlinear features. In order to keep track of of the different orders of approximation, we will apply a multiple-scale analysis in the next section.

3. Nonlinear Wave Approximation

A linear approximation of wavelike solutions of the Einstein equations is not adequate in the case of high energy or strong curvature. There is a powerful approximation method to study nonlinear gravitational waves without any averaging scheme. The method is called a “two-timing” or “multiple-scale” method, because one considers

the relevant fields in point x on a manifold M dependent on different scales [10] - [12] :

(8)

Here represents a dimensionless parameter, which will be large (the “frequency”,). So is a small expansion parameter. Further, , and scalar (phase) functions on M. The small parameter can be the ratio of the characteristic wavelength of the perturbation to the charac-

teristic dimension of the background. On warped spacetimes it could also be the ratio of the extra dimension y to the background dimension or even both. One is interested in an approximate solution of the metric and matter fields. If one substitute the series Equation (8) into the field equations, one obtains a formal series where now n runs from to, with m a constant. One says that Equation (8) is an approximate wavelike solution of

order n of the field equations if for all n. The method is very useful when one encounters

non-uniformity in a regular perturbation expansion, i.e., the appearance of secular terms. In general relativity, this will occur when high-frequency gravitational waves interact with the background metric or the curvature is strong due to the presence of compact objects. On our 5D spacetime, we expand

(9)

with the background metric and the background scalar and gauge fields. Let us consider, for the

time being, only rapid variation in the direction of transversal to the sub-manifold = constant (One could also consider independent rapid variation transversal to the sub-manifold = constant). We can now define

(10)

with. We expand the several relevant tensors, for example,

(11)

(12)

with

(13)

(14)

where the colon represents the covariant derivative with respect to the. These expressions can also be calculated on. We substitute the expansions into the effective brane Einstein equations Equation (4) and

subsequently put equal zero the various powers of. We then obtain a system of partial differential equations

for the fields and the scalar gauge fields and. The pertur- bations can be j-dependent. The Einstein equation becomes

(15)

and the equation

(16)

The contribution from the bulk space, , must be calculated with the 5D Riemann tensor

(17)

If we consider, i.e., the eikonal equation, then one obtains from Equation (15)

(18)

which in other contexts is used as gauge conditions. It turns out that the contribution from the don’t change this conditions on, if we take, which is a pleasant fact. Let us consider as a sim- plified case. Then we obtain from the gauge condition Equation (18) that only and survive. If, one proves in the 4D case that the arises from a coordinate transformation and is not a wavefront of the background. Let us consider the zero-order Equation (16). The most important contribution comes from

(19)

One also needs the Ricci tensor in Equation (16), which is given by (for)

(20)

From the Einstein equations Equation (16), one can deduce a set of partial differential equations (PDE’s) when one imposes additional gauge conditions. As a simplified model, we take, (leaving 4 independent terms), we have 7 unknown functions for the back- ground and first order perturbations: and. Here represents the background warp factor. One can also integrate the Equation (16) with respect to. If we suppose that the perturbations are periodic in, we then obtain the Einstein equations with back-reaction terms:

(21)

where we took for the RS fine-tuning and de period of the high-frequency components. One can say that the term in Equation (21) is the KK-mode contribution of the perturbative 5D graviton. It is an extra back-reaction term, which contain amplified by the warp factor and with opposite sign with respect

to the -term. So it can play the role of an effective cosmological constant. By substituting back these equations into the original equations, one gets propagation equations for the first order perturbations. In this way we obtain the set PDE’s [13]

(22)

(23)

(24)

(25)

(26)

(27)

(28)

(29)

We notice that in our simplified case of radiative coordinates, the equations for the background metric separates from the perturbations. So this example is very suitable to investigate the pertur- bation equations. For the first order gauge field perturbation we used the condition, which is a consequence, as we will see, of the gauge field equations. So can be parameterized as. The propagation equation for yields, which is expected, because the brane part of must be separable from the bulk part. We omitted for the time being, the contribution.

It is manifest that to zero order there is an interaction between the high-frequency perturbations from the bulk, the matter fields on the brane and the evolution of, also found in the numerical solution [5] . We observe again that the bulk contribution is amplified by. It is a reflection of the massive KK modes felt on the brane. The contribution of in Equation (29) disappears when. In the static case this

results in a solution (a = 1/2 in our case). This solution is of less physical significance because a distant test particle in this field will be repelled from the cylinder for [14] . The equations for the matter fields can be obtained in a similar way. The equation for the background becomes

(30)

The equation for is the same as in the unperturbed situation. For the first order perturbations we obtain ( for)

(31)

(32)

(33)

For these matter field equations one needs the condition, otherwise the real and imaginary parts of interact as the propagation progresses. From Equation (26), Equation (27) and Equation (33) we observe on the right hand side j-dependent terms, amplified by. So the approximate wave solution is no longer axially symmetric, also found by [10] . After integration with respect to j, we obtain from Equation (27) ( for)

(34)

This means that the first order disturbance () could have its maximum for fixed angle j amplified by the warp factor. If we choose for example, then the last term in Equation (34) becomes, which has two extremal values on . The energy-momentum tensor component is

(35)

This angle-dependency could be an explanation of the recently found spooky alignment of the rotation axes of quasars over large distances in two perpendicular directions.

The next step is to investigate the higher order equations in, which will provide the propagation equations of and back-reaction terms in the background field equations Equations (22), (23) and Equation (24). In this way, one can construct an approximate solution of the Einstein and scalar-gauge field equations and one can keep track of the different orders of perturbations.

4. Conclusion

A nonlinear approximation of the field equations of the coupled Einstein-scalar-gauge field equations on a warped 5D spacetime is investigated. To zeroth order in the expansion parameter it is found that the evolution of the perturbations on the brane is triggered by the electric part of the 5D Weyl tensor and carries information of the gravitational field outside the brane. The warp factor in the nominator in front of the bulk contributions will cause a huge disturbance on the brane and could act as dark energy. It turns out that the first order disturbances are no longer axially symmetric. This means that wavelike disturbances in the energy-momentum tensor com- ponents can have preferred directions perpendicular to each other. This could be an explanation of the alignment of the preferred directions of the quasar polarization axes.

Conflicts of Interest

The authors declare no conflicts of interest.

Cite this paper

*Journal of Modern Physics*,

**7**, 501-509. doi: 10.4236/jmp.2016.76052.

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