Advances in High Energy Physics

Volume 2015 (2015), Article ID 404508, 10 pages

http://dx.doi.org/10.1155/2015/404508

## Critical Combinations of Higher-Order Terms in Einstein-Maxwell Theory and Compactification

^{1}National Institute of Technology, Gifu College, Motosu-shi, Gifu 501-0495, Japan^{2}Graduate School of Science and Engineering, Yamaguchi University, Yamaguchi-shi, Yamaguchi 753–8512, Japan

Received 27 August 2015; Accepted 1 November 2015

Academic Editor: Chao-Qiang Geng

Copyright © 2015 Nahomi Kan and Kiyoshi Shiraishi. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.

#### Abstract

We discuss the role of a particular combination of higher derivative terms in higher dimensional theories, particularly in the background of spontaneous compactification. Two classes of theories are proposed in this paper. The first model as a generalization of the critical gravity with the Maxwell field could have a de Sitter solution. We consider the Lanczos-Lovelock term and Horndeski term as well as the higher-order Maxwell term for the second model, which contains a possible longer expansion time for the inflationary phase. It is interesting that both models can be regarded as the generalization of the Randjbar-Daemi, Salam and Strathdee (RSS) model and give the well behavior for inflation stage under the specific assumptions.

#### 1. Introduction

Over several years, the gravitational theory with higher derivative terms [1, 2] has been a highly interesting subject studied in physics. The treatment of Einstein gravity with perturbative field quantization naturally leads to the inclusion of such nonlinear terms in the spacetime curvatures for effective actions.

The generalization of Einstein gravity has been developed extensively by many authors. The Lanczos-Lovelock gravity [3–6] (for a review, see [7]), which is dictated by effective action with the dimensionally continued Euler forms, is defined in a generic dimensional spacetime, and it describes a massless spin-two fluctuation despite the existence of higher-order terms in its action. About a few decades ago, it was discovered that the effective field theory arising from string theory involves similar terms at least for the lowest-order correction to the Einstein-Hilbert term [8, 9].

The other specific extension is found in the study on the so-called critical gravity [10–12] (although the word “critical” originally implied the emergence of Log gravity [13–15]). In this gravitational theory, the behavior of spin-two modes is described by the Lagrangian of a special combination of higher-order terms in the Ricci tensor and the scalar curvature. There is a ghost field but no spin-zero mode in this theory. In the three-dimensional spacetime, the model governed by a similar Lagrangian expresses the new massive gravity [16, 17].

In this study, we consider incorporation of the Maxwell fields to the (next-to) critical gravity, which has been studied under the assumption of the maximally symmetric background spacetime. The higher derivative theory for the other type of background fields is worth studying. Inclusion of a nonvanishing flux field brings about partial compactification with a maximally symmetric extra space and might provide an interesting scenario for a very early stage of the universe.

The assumption of the partially symmetric solution could yield another possibility. It is feasible to attach the other type of higher-order terms to the Lagrangian which realizes the spontaneous compactification. Due to the symmetry, the use of the Riemann tensor is possible in the additional terms, which are expressed by special combinations of Gauss-Bonnet terms and Horndeski’s generalized Maxwell term [18]. These terms induce a second-order field equation displaying the cosmological evolution of the background geometry (the applications of the Horndeski’s vector-tensor theory have been discussed previously in four-dimensional [19, 20] and in six-dimensional cosmology [21]).

This paper is organized as follows. In Section 2, we build the Lagrangian of our first model, which involves the quadratic terms of the Ricci tensor, the Ricci scalar, and the two-form flux field, in a similar way as revealed before in the study of critical gravity. The spontaneous compactification in the first model is studied in Section 3 and cosmological solutions are examined in Section 4. In Section 5, we present the second model containing the quadratic term of the Riemann tensor. We also investigate the cosmological solution qualitatively in this model. The last section is devoted to the summary and further research prospects in this area of study.

It is to be noted that throughout this study, we deal with our models at the classical level only.

#### 2. A Critical Modification of Einstein-Maxwell Theory

In the study on critical gravity, it is found that the Lagrangian of the specific combination of curvatures yields a spin-two massless graviton and a ghost mode; there appears no scalar mode as in Einstein gravity. In this section, we propose a model of higher-order extension of the Maxwell-Einstein theory. We will follow the method for constructing the Lagrangian examined in our previous study [22, 23]. In [22, 23], we constructed the action of higher derivative pure gravity which admits the (anti-)de Sitter solution. In similar sense, we manage to construct the model with higher-order terms in which background fields satisfy the Einstein equation in the presence of the Maxwell field in this paper.

First, we start with the action for the Einstein gravity and electromagnetism in dimensions: where and denote the scalar curvature obtained from the metric and the cosmological constant, respectively. The field strength is defined by with a vector field and . The suffixes vary over .

Apply the variational principle to the action results in the following equations of motion: with where and

Next, we construct a Lagrangian for our model as follows: where Note that the solution of is the solution for the equation of motion derived from , provided that the field equation for the vector field is satisfied (though the stability is not necessarily guaranteed). (Generally speaking, we can add the term to our Lagrangian, but we restrict ourselves to the case without such a term in the present paper.)

The Lagrangian can then be written as

Incidentally, we can pick up some “critical” cases: if , the contribution of the cosmological constant is zero in the -dimensional spacetime; if , the Einstein-Hilbert term is absent from the -dimensional action; and if , the pure Maxwell term is absent from the -dimensional action.

We should note that the auxiliary field method [14, 16, 17, 23], which can be used in critical higher-order gravity, also leads to the additional terms such as where is an auxiliary symmetric tensor field and . Varying the auxiliary field , we obtainor, solving this equation with respect to , we get Therefore, one can see the equivalence between the Lagrangians, and . We can derive the linearized field equation using the action

Now, we investigate the behavior of the linear fluctuations around the background geometry, which satisfies . We decompose the metric as follows: The indices are raised and lowered by the background metric, . Then, the trace of the fluctuation is expressed as For convenience, we write down the curvature tensors up to the linear order in here as [24]where the nabla stands for the covariant derivative and the barred symbols show that they are constructed from the background metric, .

Assuming the background field satisfies , we can use to obtain the field equation with a linearized order:Noting that is in the linear order (), we have used the condition for the background field.

The generalized Maxwell equation in the linear order of fluctuations takes the form where .

The linearized equation obtained from (9) is

The important observation is that, using (9), the field equation (15) becomesIn the -dimensional Minkowski vacuum, this equation is just the Fierz-Pauli equation [25] for the spin-two wave with mass-squared . Therefore, we recognize that corresponds to the massive ghost field. The postulation of no tachyonic ghost requires in the present model.

The linear fluctuation from the background fields can be investigated by using the above equations. In the next section, we consider the solution for spontaneous compactification of spacetime as the background.

#### 3. Spontaneous Compactification in Critically Modified Higher-Order Einstein-Maxwell Theory

In this section, we study the partial compactification of space with a nontrivial flux in our model. The extra dimensions are considered to be compactified into a sufficiently small size. A partially symmetric solution in our model describes compactification of the form , where is the dimensional Minkowski spacetime and is a two-dimensional sphere, as in the work of Randjbar-Daemi, Salam and Strathdee (RSS) [26], where is considered. We consider the solution for the flat dimensional spacetime and study its classical stability in this section, though other symmetric spacetimes are also interesting. Our notation is that the suffixes run over and the suffixes are used for the extra dimensions of and .

As stated in the previous section, the solution for and is a solution in our model. A suitable ansatz for the flux field is where is the antisymmetric symbol and the constant is the strength of the two-form flux. (It can be checked that this configuration is the solution of our model.) This monopole flux yields the relation,

Then, the equation, , can be decomposed tofor the spacetime of a direct product. As for the flat dimensional spacetime, where , we consider a fine-tuning of the parameters asAnd, therefore, the solution for the background fields reads

Substituting this compactified background solution into (18), we obtain

To show the complete particle spectrum for the ghost field is rather complicated, but we can see that the lowest mass of the ghost is for symmetric tensor fields (which does not couple to the Ricci curvature of the extra space) and vector bosons of the Kaluza-Klein origin (which come from the zero modes of the Lichnerowicz operator on , ). It is also remarkable that the other graviton and vector field fluctuations are absent in the linearized equation (24).

Thus, taking the analysis by RSS for other fluctuation modes [26] into account, in the classical and linearized analysis, we find that the RSS background solution is stable if , because there is no growing mode. (Of course, there remains the problem of nonlinear instability and the ghost problem in quantum physics.)

Before closing this section, we note that the effective dimensional Newton constant, which can be found by the coefficient of the Ricci scalar of the dimensional spacetime in the action, is not affected by the higher-order terms in our model and is independent of , if the conditions on the background fields (22) and (23) are satisfied. (If we express the -dimensional Ricci scalar as , where is the Ricci scalar of the dimensional spacetime, the coefficient of in the Lagrangian (7) is found to be .) It might be related to the absence of the graviton and the ghost modes in (24) at the linearized level mentioned above.

#### 4. De Sitter Solutions and Cosmology in the Model

In this section, we perform the analysis on the stability of the compactification and the cosmological solution in our model. We consider an effective potential for the radius of extra space [27] in order to study them.

We can express the Riemann tensor of the as where denotes the radius of the compactified sphere . Then, (21) with impose [26] where the first equation represents the fine-tuning condition between the parameters.

The effective potential as a function of , the scale of the extra space, is obtained by replacing the background fields with functions of in such that and . The effective potential for the RSS model is calculated from and is given as Therefore, the effective potential for our model of which the Lagrangian is described by (7) is with . A minimum of the potential is found at and attains . The stability of the radius of the extra sphere is determined by the sign of the second derivative of the potential: If and , the scale is found to be stable. We also find that it is impossible to create another potential minimum satisfying by any fine-tuning of in the model.

At a large value of , can be indefinitely negative provided that . In this case, the -dimensional cosmological constant becomes negative. This may not indicate instability of compactification against a large fluctuation, because the higher derivative terms induce a coupling between the compactification scale and the first and second derivatives of an expanding scale factor for the rest of the space.

Therefore, we investigate the cosmological equation including the dynamical scale factor and the compactification scale. The metric is usually assumed as where denotes the radius of the compactified sphere and is the line element in the unit sphere. For the maximally symmetric dimensional space, the line element is denoted by here, and its Riemann tensor is normalized to with , where . The symbol is the scale factor for the dimensional homogeneous and isotropic space.

The Riemann curvature is computed with the metric as where the dot denotes the derivative with respect to the cosmic time .

Now we can obtain the effective action of the scale factor, , and the compactification scale, , for the RSS model as where the overall constant which comes from the volume of the space has been omitted. The action written after the symbol “” has been integrated by parts.

The effective action for our model can be written, by adopting the auxiliary fields, as where we set , , and . Here, the equations of motion are omitted, but they can be obtained from the above action. (The Euler equations can be obtained from the action using the command EulerEquations in the add-on Calculus “VariationalMethods” for Mathematica [28].)

We seek for the de Sitter () solution, where , with constant , and constant are taken as an ansatz. In this case, all the equations of motion become algebraic equations. With the ansatz, the auxiliary variables are expressed as Substituting these auxiliary relations to the other equations, we obtain the following two equations at last:

The two sets of the solution for and can be found; one isand the other isThese values for solutions are the same as those of the RSS model [29], as expected (if ). In both cases, the values for , , and are equal to zero.

Since the simultaneous equations ((36), (37)) are fourth-order algebraic equations, there are two more sets of solutions (in general, the values for , , and are not zero for such solutions) at the most. We may infer that for sufficiently small value of , only two original solutions ((38), (39)) are real solutions. For , only two real solutions ((38), (39)) exist for . As a model of the universe, the multiple de Sitter phases would have some significance in cosmology.

We now study the behavior of the small fluctuations around the above exact solutions. In the neighborhood of (i), we set, and so on. Then, the linearized equations of motion can be expressed as Note that, for , the above equations give , , and , which are equivalent to the equations for the cosmology of the RSS model [29].

The oscillatory behavior of as well as is already interesting enough. The variables , , and oscillate with a different frequency from that of , as seen from (42) and (43). (Note that the angular frequency of the oscillation of is the square root of in (30).) Thus, the tuning of the initial conditions provides enough time for accelerating expansion and a sufficient inflation can be achieved, though we cannot predict the choice of the initial state in the present classical analysis of the model.

The analysis of the perturbation from (ii) can be performed and it results in finding exponentially growing modes, as found in [29], though we omit the indication of equations here. A certain fine-tuning could give enough expansion time for a sufficient inflation as the de Sitter phase also in this case.

#### 5. Spontaneous Compactification in Lovelock-Horndeski-Nonlinear Maxwell Theory

In the solution for the spontaneous compactification in previous sections, one can deduce the following relation in the background fields:Similar to the consideration in the previous sections, we come up with an idea that the Minkowski compactification of the RSS model is attained in a higher derivative theory if the relation (46) is reflected in the higher-order correction term.

We then propose an additional higher-order term where generalized Kronecker’s delta is defined by Now, we write model 2 by the Lagrangian (therefore, we call the previous model model 1): Note that consists of the Lanczos-Lovelock Lagrangian (Gauss-Bonnet term) [3–6], the Horndeski’s vector-tensor term [18], and a nonlinear Maxwell term.

It is easy to see that adding to the RSS Lagrangian yields no modification of the linearized equation of motion on the RSS background fields after gauge fixing. Therefore, the Kaluza-Klein modes remain unchanged from those in the RSS model. It is worth noting that the effective dimensional Newton constant in model 2 is not affected by the value of .

Now, we study the cosmological evolution of the classical background in the model. Although the Kaluza-Klein cosmologies with the Gauss-Bonnet term or the generalized Euler invariant have been investigated in many studies including [30–35], the case with the RSS-type compactification with the Gauss-Bonnet term has been studied only in a few papers including [36]. (The compactification with the Horndeski Lagrangian has been considered by one of the present authors [21].)

As previously considered, we characterize the cosmological background by Then, the Lagrangian reduces to and we obtain the following action for and : Again, we omit the exposition of equations of motion here.

We first explore the de Sitter phase or the maximally symmetric product spacetime. To find this, we set , , and , where and are constants. We then obtain the simultaneous algebraic equations as follows: Of course, the solution (i) (38) is a trivial solution of the above equations, while (ii) (39) is not a solution for . One solution of the simultaneous equations ((53), (54)) with exists for all positive . The value of increases with the value of . The existence of the de Sitter phase with large values for and is suitable for the possible inflationary phase.

Next, we draw the phase diagram of the compactification scale . We consider the case with and . Figure 1 shows the phase space spanned by and for . The small arrows in the figures indicate the flow in the phase space. One can see that is an attractor and the area of the attracting region increases with the value of . (If ordinary matter is added, the dissipative motion becomes more apparent in an expanding era [37].) We conclude that an appropriate choice of the initial condition, which governs the flow passing through the branch point given by the de Sitter solution of (53) and (54), might result in a longer expansion time.