Research Article  Open Access
NMC and the FineTuning Problem on the Brane
Abstract
We propose a new solution to the finetuning problem related to coupling constant of the potential. We study a quartic potential of the form in the framework of the RandallSundrum type II braneworld model in the presence of a Higgs field which interacts nonminimally with gravity via a possible interaction term of the form . Using the conformal transformation techniques, the slowroll parameters in high energy limit are reformulated in the case of a nonminimally coupled scalar field. We show that, for some value of a coupling parameter and brane tension , we can eliminate the finetuning problem. Finally, we present graphically the solutions of several values of the free parameters of the model.
1. Introduction
The viability of an inflationary scenario and the constraints on the inflationary model are profoundly affected by the presence of NMC (nonminimal coupling) and by the value of the coupling constant [1]. The analysis of the various inflationary scenarios considered in the literature usually leads to the result that NMC makes it harder to achieve inflation with a given potential that is known to be inflationary for .
Among the various models of the inflationary scenario, Linde’s chaotic model [2] has been regarded as a feasible and natural mechanism for the realization of inflationary expansion. This model still has a serious problem; that is, one has to finetune the selfcoupling constant of the inflaton which is unacceptably small to have a reasonable amplitude of the density perturbations.
On the other hand, Fakir and Unruh (FU) proposed a way to avoid finetuning by introducing a relatively large nonminimal coupling constant in the context of the chaotic inflationary model. According to their results, the large value of , that is, order of , allows us to have a reasonable value for the coupling constant . Thus, the FU scenario remains a reasonable model of the inflationary scenario [3].
Nevertheless, the feasibility of inflation has been also investigated in alternative theories of gravity, for example, the BransDicke scalar tensor theory [4, 5], and nonminimal coupling theories of gravity [6]. Furthermore, the analytical study of the same brane model with a nonminimally coupled scalar has also been studied in [7, 8].
Recently there was an extensive discussion of Higgs inflation in the theory with the potential and nonminimal coupling to gravity [9], with the Higgs field playing the role of the inflaton field. The main idea was to introduce a large nonminimal coupling of the Higgs field to the curvature scalar, and after that, one can make a transformation from the Jordan frame to the Einstein frame to render the potential of the Higgs field sufficiently flat to support inflation. The effect of this coupling is to flatten the SM potential above the scale thereby allowing a sufficiently flat region for slowroll inflation [10].
There has recently been a revival of the idea that inflation based on scalar fields which are nonminimally coupled to gravity can account as a way to unify inflation with weakscale physics [11]. However, it has been suggested that such models are unnatural, due to an apparent breakdown of the calculation of HiggsHiggs scattering via graviton exchange in the Jordan frame [12]. On the other hand, it was shown [13] that Higgs inflation models are in fact natural and that the breakdown does not imply new physics due to strongcoupling effects or unitarity breakdown but simply a failure of perturbation theory in the Jordan frame as a calculational method. Also, it was suggested that Higgs inflation is a completely consistent and natural slowroll inflation model when studied in the Einstein frame [13].
In addition, a new class of models of chaotic inflation in supergravity was proposed in [14]. Moreover, this new class of supergravity models can describe an inflaton field which is nonminimally coupled to gravity, with coupling [15]. In this class, in order to make these models consistent with observations, there is no need to go to the limit ; a very small positive value of is quite sufficient.
In this work, we are interested in an inflationary model in the braneworld model with a quartic potential of the form in the Einstein frame with a nonminimally coupled Higgs scalar field in relation to recent observations [16]. Using the conformal transformation techniques [17], the slowroll parameters with are obtained, and we show that we can eliminate the finetuning problem related to the coupling constant of the potential for some value of a coupling parameter and brane tension . We will also show that, depending on the parameters of the model, one can cover a significant part of the space of parameters () allowed by recent observational data.
The plan of the paper is as follows. In the next section, we recall first the conformal transformation techniques. In Section 3, we study the RS2model with a nonminimally coupled Higgs scalar field. In Section 4, we present our results for a quartic potential in the Einstein frame on the brane. A conclusion is given in the last section.
2. Conformal Transformation Techniques
Recently, the use of conformal transformation techniques has become widespread in the literature on gravitational theories alternative to general relativity and in particular on nonminimally coupled scalar fields to the spacetime Ricci curvature scalar. As it is well known, if only one scalar field is nonminimally coupled, then one may perform a conformal transformation to a new frame in which both the gravitational portion of the Lagrangian and the kinetic term for the (rescaled) field assume canonical form [18].
Consider general scalartensor theories (STT), in dimension with the metric (to be called the Jordan conformal frame), for which the gravitational field action is written in the following form [17]: where is positive definite. is a gravitational constant in dimensions.
The nonminimal coupling associated with the renormalization counterterm takes the following form: Note that this term corresponds to a nonminimally coupled scalar field with an interaction term of the form , where is a dimensionless coupling constant. Minimal coupling corresponds to , where We may further parameterize the following, in terms of a Planck mass in dimensions: For , we have . In the sign conventions of (2), a conformally coupled field has We may use a conformal transformation of the metric, defined as where is determinant of the metric in the Einstein frame, and a new field appears which is related to the field via [17] The combination of (8) is always nonzero, because we have only considered models in which is positive definite and real.
In terms of new variables, the action of the model is given by where we have introduced a transformed effective potential The action equation (9) is similar to that of with a minimally coupled scalar field in addition to arbitrary . This has also both the canonical EinsteinHilbert form and the canonical kinetic term for the scalar field.
In the next section, we will clarify the link between the conformal transformation techniques and the slowroll approximation. We prove that slowroll inflation in the physical Jordan frame implies slowroll inflation in the Einstein frame.
3. NMC and the SlowRoll Approximation to Inflation
We start this section by recalling briefly some foundations of RandallSundrum type 2 braneworld model with a nonminimally coupled bulk scalar field via an interaction term of the form . We will use here the conformal transformation techniques introduced in Section 1 in the case of . In this scenario, our universe is considered as a 3brane embedded in fivedimensional antide Sitter spacetime (AdS5), where gravitation can propagate through a supplementary dimension. One of the most relevant consequences of this model is the modification of the Friedmann equation for energy density of the order of the brane tension or higher.
The field in the Einstein frame with is not canonically normalized. In effect, the canonically normalized inflaton field can be related, via (8), to the field as follows: The fourdimensional Planck scale is given by [19] where .
In doing the slowroll analysis, we should note that slowroll approximation puts a constraint on the slope and the curvature of the potential. This is clearly seen from the field expressions of and parameters. Thus, in the Einstein frame, it is and not that has a canonical kinetic term. Therefore, the slowroll parameters are where and is the brane tension. We signal that the slowroll approximation takes place if these parameters are such that and inflationary phase ends when or are equal to one. Before proceeding, it is interesting to comment low and high energy limits of these parameters. Note that at low energies where , the slowroll parameters take the standard form. At high energies (our case) , the extra contribution to the Hubble expansion dominates.
Another important characteristic inflationary parameter is the number of efolding defined by [19] The small quantum fluctuations in the scalar field lead to fluctuations in the energy density and in the metric. For these reasons, we define the power spectrum of the curvature perturbations by [20] The ratio of tensor to scalar perturbations is In relation to , the scalar spectral index is defined as [20] Another perturbation parameter spectrum quantity is the running of the scalar index , defined as From now on, we set and we use (11) to calculate the slowroll parameters as function of as follows: where and where and . This does not change the direction of rolling but modifies the velocity of the field such that with heavier rolling mass the motion becomes slower (smaller and ) as indicated by (19) and (20). Similarly, we can find the number of efolds by where the subscripts and end are used to denote the epoch when the cosmological scales exit the horizon and the end of inflation, respectively.
The power spectrum of the curvature perturbations and the running of the scalar index becomes, respectively, In what follows, we will apply the above braneworld formalism with a quadratic potential in the Einstein frame to derive perturbation spectrum in relation to recent Planck data [16]. This potential has been recently studied in [15] for the standard inflation.
4. Perturbation Spectrum for a Quartic Potential
The coupling constant is often regarded as a free parameter in inflationary scenarios. This view arises from the fact that there is no universal prescription for the value of . Indeed, some prescriptions for do exist in specific theories, although they are not widely known and they depend on the nature of the scalar field and on the theory of gravity [21].
On the other hand, the prevailing point of view in the literature on inflation is that the coupling constant is a free parameter and that the values of that which are acceptable are those that, a posteriori, make a specific inflationary scenario viable [22]. Thus, in the context of cosmology, it has been recognized that nonminimal fields could be employed to solve some problems associated with inflation, for example, the finetuning problem related to coupling constant . Note that more inflationary scenarios have studied this problem; for another type of models, see [23, 24].
We will consider the case of a quartic potential, in the Jordan frame, , which leads to the Einstein frame potential as follows: The model with , which is equivalent to considering the inflaton Higgs field to be minimally coupled to gravity, is singled out by its simplicity and the potential is very flat. In this context, one can also consider the slowroll parameters to study the spectrum of the perturbation. The two first parameters are given for this model by where On the other hand, one can derive the number of efolding as Although we have analytic results for slowroll parameters, it is not easy to solve them to obtain at which the observables , , and should be evaluated. Instead, we proceed numerically by finding and then going efolds back to obtain while making sure that the slowroll parameters remain small in this range of .
Moreover, the combination of Planck + WP data, with the pivot scale chosen at , gives the following results [16]: In the following, we will study different regimes of coupling . Our results will be compared to observations and the coupling effect on perturbation inflationary spectrum will be studied.
4.1. Minimal Coupling Case
We investigate in this case the simplest chaotic potential of the form in the Jordan frame with a minimally coupled scalar field . Equation (26) gives the integrated expansion from to as After that, we calculate the value of the scalar field at the end of inflation, in terms of and . Using this, (31) for can be solved to give , where is the value of the scalar field efoldings before the end of inflation. Finally, starting from (30), we can plot the variations of physical quantities for various values of (see Table 1).

We remark that, in Table 1, for different values of , we obtain the very small values of the coupling constant which introduces the existence of the finetuning problem. These results coincide with the results of the chaotic inflation in the standard case. We remark also that the parameters and coincide with the observation values except for . Note that, in this case, it does not show the effect of the brane tension because it is simplified in the calculation.
In what follows, we will show that the addition of the parameter (where ) and the brane tension has a significant impact on the spectrum of the model and gives solutions to the finetuning problem and the inflation can occur successfully.
4.2. Conformal Coupling Case
In this section, we limit the discussion to the model when ( is the fivedimensional conformal coupling) where we use the potential in the Einstein frame of the form .
Figure 1 shows the variation of the scalar spectral index as function of for different values of the coupling constant . We observe that values of of about may have a cover interval which coincides with the observation data for , where the finetuning problem is solved. We also note that, for small values of , for .
Figure 2 shows the variation of the ratio with respect to for different values of the coupling constant . We show that is a decrease function with for the different values of . We have also shown that is consistent with the observation data for . We emphasize that, for small values of , the is negligible.
Figure 3 shows the variation of the running of the scalar spectral index as function of for different values of the coupling constant . We show that the running of the scalar spectral index is small and negative which is consistent with recent observation data. We also remark that, for small values of , the does not exceed (.
Note that, in order to obtain the value of the power spectrum of the curvature perturbations for , one should take the following values , , and .
Finally, in this case, we have shown that by variation of the free parameters and , the results reviewed by the value of are compatible with the observational data for the value of where the finetuning problem is solved and the inflation can occur successfully. For example, for , , and , we find the central value , , and .
4.3. General Case
In this case, we will discuss possible physical implications of the solutions in the case of and . The motivation is to examine whether this model coincides with the observation for and .
In Figure 4, we present the variations of scalar spectral index according to the value of the coupling constant for different values of . We show that in the two regions decreases when increases and we can have a range of for small values of where the four curves are almost confounded which is in agreement with the observations.
Figure 5 shows the variation of the ratio with respect to for different values of the coupling constants . We can remark in Figure 5 that the ratio increases with respect to for two regions and which is in agreement with recent observation data. On the other hand, for values of of the order of , which is outside the observed region.
In Figure 6, we present the variations of running of the scalar spectral index according to the value of the coupling constant for different values of . We emphasize that is positive and not consistent with the observation for different values of and ; see (29).
In summary, we note that, in this section, with potential of the form , we find a more precise interval of the nonminimal coupling for assisted inflation and the parameters and are in agreement with observation for the free parameters of the model.
5. Conclusion
In this paper, we have studied a quartic potential of the form in the Einstein frame with the Higgs field nonminimally coupled to gravity for the different cases of and for arbitrary values of the parameters and . The slowroll parameters in the brane are reformulated in the case of a nonminimally coupled scalar field. We have shown that, by changing parameters of these models, one can cover a significant part of the space of the observable parameters (; ;) allowed by recent observational data for the different cases of . We have also shown that, in order to avoid finetuning of the potential, the introducing of a relatively nonminimal coupling constant of the order of unity is quite sufficient to allow us to have a reasonable value for the coupling constant for . In addition, we have examined the properties of the new case. The case of predicts undesirable values of (; ;) with recent observational data. Finally, there has been a great deal of work on NMC in the inflationary models; this paper justifies certain methods used, solves some of the problems posed, and proves that inflation, with nonminimal coupling, can occur successfully for the simplest inflationary models in braneworld.
Conflict of Interests
The authors declare that there is no conflict of interests regarding the publication of this paper.
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Copyright
Copyright © 2014 A. Safsafi and M. Bennai. 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}.