Research Article | Open Access

Sergey G. Rubin, "How to Make the Physical Parameters Small", *Advances in High Energy Physics*, vol. 2020, Article ID 1048585, 9 pages, 2020. https://doi.org/10.1155/2020/1048585

# How to Make the Physical Parameters Small

**Academic Editor:**Torsten Asselmeyer-Maluga

#### Abstract

We study the evolution of the physical parameter values defined at the sub-planckian energies to values at low energies. The Wilson action is the basis of the research. The presence of the compact extra dimensions has two consequences. The positive point is that the integration over extra dimensions is a promising way to substantially reduce the parameters to be comparable with the observational values. On the other hand, the discreteness of the energy levels of compact extra dimensions complicates the analysis. This difficulty can be overcome with the truncated Green functions.

#### 1. Introduction

It is assumed that the physics is formed at high energies [1, 2]; the widespread idea on the inflationary processes at the early universe is the well-known example. Absence of the quantum gravity forces is working at the sub-planckian energies as the highest scale. The purpose of future research is to discover or guess the structure of theory at the sub-planckian scaleâ€”its dynamical variables, symmetries, and parameter values [3, 4].

The evident difficulty is that we live at low energies, where the values of the observable physical parameters could strongly deviate from their initial values [5]. Moreover, the same structure of the Lagrangian at high energies could be different from those at low energies due to the quantum corrections, for example.

One of the aims of the fundamental physics is to postulate a Lagrangian depending on primary parameters and fix them using their connection with observational values. This means that we have to calculate the parameter values at low energies starting from those at high energies [6â€“8]. The well-known Wilson approach [9] is accommodated for this purpose, and this idea is used in this paper.

The parameters at sub-planckian energies are usually supposed to be of the order of the Planck scale [10], much larger than the observable values at the present time. At the same time, the variation of the parameter values with energy is proportional to coupling constants which are usually assumed to be small compared to the Planck scale. This means that there is no proper way to connect the parameters at both scales, and hence, new mechanisms should be involved which is the essence of the hierarchy problem [11, 12].

The idea of extra dimensions is very popular now and is used in the solution to many problems [11, 13, 14]. It is shown here that the insertion of an extra space facilitates the connection of high energy Lagrangian structure and the low energy one. This is shown in a study done in our first article [15]. At the same time, the extra space inclusion complicates the calculations, especially if the extra dimensions are compact.

In the previous paper [15], we studied the role of the compact extra dimensions on the parameter variation with energy. Starting from a moderate scale, we have shown that integration over additional coordinates can lead to a strong change in physical parameters from a 4-dimensional point of view. It is also possible to adjust them to the observable values with the help of the inhomogeneous extra dimensions [16].

In this paper, we continue discussion starting from the sub-planckian energy scale where the excitations of the extra space metric can not be neglected. We start with the analysis of running constants at the high energies [17] in the spirit of the Wilson action. The truncated Green function is used to neutralize the discreteness of the Kaluza-Klein spectra. As is shown below, the corrected parameters (the Lambda term is an important exception) differ slightly from the initial ones if coupling constants are assumed to be small. This means that this mechanism is not very effective and can not be responsible for the parameter variation in many orders of the magnitude. It is also confirmed that integration over the extradimensional coordinates could be able to shift the parameter values to the observational range.

The analysis made in this paper is based on the toy modelâ€”scalar-tensor gravity [18, 19] with compact extra space. We start from the scalar field theory at high energies (small distances) and find the mass of the scalar field oscillations at lower energy scales.

The research is based on the multidimensional variant of the gravity. The interest in theories is motivated by inflationary scenarios starting with the work of Starobinsky [20, 21] where 4-dimensional metric is used. Some models in 4-dim space that satisfies the observable constraints are considered in Refs. [19, 22]. New branch which uses the Horndeski equations is also developed nowadays [23]. The model used here is based on the 4-dim space endowed by extra dimensions.

In the next section, we check a statement on the smallness of the quantum corrections in the presence of the compact extra dimensions with its discrete spectrum. The Wilson approach is modernized, because it is not clear how to extract an â€śinfinitely small energy layerâ€ť in this case.

#### 2. Parameters Renormalization in Presence of Extra Dimensions

We use the Wilsonian approach to study the renormalization of the physical parameters in coarse of slowing down from high to small energies. Primary parameters are assumed to be fixed at high energies, in our case. There are several scales that influence the dynamic of the parametersâ€”D-dim Planck mass , the electroweak scale , the size of local extra space , and the scale . The relations between scales are assumed to be as follows:

In this section, it will be shown that the perturbative procedure of the renormalization cannot help in a significant reduction of the physical parameters, the cosmological constant is the important exception.

Here, we study the energy dependence of the parameters in the spirit of the Wilson approach by defining physics at the highest energies. Descending to the electroweak scale or lower is the necessary step. This process is accompanied by a variation of physical parameters due to quantum fluctuations. It appears to be not easy to shift energy to small values on the basis of pure gravity. Insertion of scalar field(s) improve the situation [15, 24].

Consider the action of the scalar field and gravity acting in a D-dim space. The purpose of the study is to elaborate a way of renormalization of physical parameters in the presence of the extra space. For this, the scalar field is considered. Given the complexity of the study, the influence of the scalar field on the metric is ignored. The opposite case has been discussed in [25] with the specific choice of parameters that leads to a correct inflationary model.

The metric is chosen in the form

It is assumed that the de Sitter stage is the result of other fields affect like the Higgs field [26] or the gravity with higher derivatives [21].

Let us estimate the Hubble parameter value. We start from the scale and descend to lower energies. According to the model of chaotic inflation [27], the Hubble parameter relates to the energy density as . Hence, the characteristic value of the Hubble parameter is . On the other hand, we consider all physical parameters (including the mass ) being of order of . Therefore, according to inequalities (1).

The equation of motion for the homogeneous space in de Sitter space is the following

It is seen that plays the role of friction and can be omitted if . In this case, equation (5) describes the motion of the oscillator without friction in the 4-dim Minkowski space, the Green function of which is well known. This fact is widely used by the inflationary models to terminate the inflationary stage.

The generating functional for action (2) at the intermediate scale plays the central role in the Wilsonian approach. The extra space is supposed to be maximally symmetric; its radius and the corresponding energy scale are related as . The functional (6) is the result of integrating out quick modes of the scalar field. The D-dimensional Planck mass is considered as the maximal energy scale in the rest of the article.

The physical parameters at the scale are of the order of . The reason for such choice is that high-energy quantum corrections from the scales to the highest scale are assumed to have been taken into account in expression (6).

Next, two subsections are devoted to discussion on the energy shifting from high values to small ones with the subsequent parameter renormalization in the presence of the extra space.

Let us clarify the notion â€śscale of integration.â€ť There is no problem to think in terms of space scale or the energy scale with the relation in 4 dimensions [28]. The energy scale is also expressed in terms of the euclidean wave vector , . The presence of local extra dimensions complicates these relations due to the discreteness of their energy levels. There are two kinds of the scalar field excitations in this caseâ€”one of them is represented by the waves along the four dimensions. The second set of the excitations in the compact extra dimensions is discrete. The correspondence between the energy of excitations in compact space and the space scale is for 1-dim extra space [29]. Suppose now that we wish to integrate over â€śvery thinâ€ť momentum layer in the 4 large dimensions. Immediate question isâ€”which of the energy states related to the extra dimensions should be taken into account also? If a chosen energy interval does not contain any discrete level , we should forget about integration over the extra space modes. We should keep them in mind only in those cases when . Therefore, the differential equations that describe the renormalization flow of parameters cannot be applied in this case.

Let us start with the standard Wilsonian procedure and formally divide the field into quick and slow parts

The quick modes relate to an energy interval which is not obligatory infinitesimally small.

Substitution (7) into (6) gives the generating functional in the form (the units are used in the rest of the paper) where

Here, we have taken into account orthogonality of and .

The way to integrate out the field from (8), provided that the coupling constant is small, is well known (see for example textbook [28]). The result of integration over quick modes can be written in the Euclid space as [28, 30].

Here, the generating functional in the Euclid space is a function of an external current . Integration over small deviations around the classical part of the field gives

The set is a set of eigenstates that were integrated out. The complex index where is the wave vector in the 4-dim Euclidean space, and marks eigenstates in the compact extra space and represents a discrete set. is the truncated Green function discussed in the Appendix. This Green function is cut both from UV and IR sides because the integration over finite energy interval is assumed.

Let us suppose that we have integrated out all discrete modes for which . This means that we are disposed at the energy scale is with space scale and the 4-dim mode of the energy excitation

Now, we have to choose next coarse-graining space scale and subsequent energy shift. We define it by the algebraic equation

The last expression follows from (15). The meaning of (16) is as follows: the selected integration layer relates to one and only one number of energy state by definition. The size of the 4-dim energy layer is according to relations (15) and (16). Therefore, the contribution of one step of the coarsening is as follows

The first term in the sum represents the contribution of all modes that are quick in the 4-dim space. The last term includes all 4-dim modes containing only one excitation of the extra dimensions. All these excitations contain wavelengths in the interval . Manipulations with the expressions similar to (18) are discussed in Appendix A in light of the truncated Green functions calculations.

Let us fix scales for the following discussion and estimations. Let , the extra space size is , and the initial energy scale is . Therefore, the energy layer is much smaller than . In this case, summation can be approximated by integration with appropriate accuracy.

Now, we will show that correction to the mass also contains the small parameter and hence is small. To verify this, let us estimate quantum corrections produced by terms proportional to . The latter can be extracted from (11), (12) and has the form

Receipt (12) with instead of leads to the quantum correction to the potential in the first multiplier of expression (8). Therefore, the correction to the scalar field mass equals and is small if the coupling constant is small. The truncated Green function has the form (see Appendix A)

Here, and is the running energy scale. Substituting the Green function (22) into the expression (20), we obtain the quantum correction to the scalar field mass.

The summation over layers gives

According to (22), the large parameter is canceled and the quantum correction appears to be proportional to the coupling constant . All other values like are smaller than unity () and does not spoil this conclusion.

The expression (21) represents the mass difference between observations at two energy scalesâ€” and . Expression (23) is obtained by the integration over all layers in the energy interval . The lower boundary is chosen because there are no KK excitations below . Renormalization of the KK masses due to the quantum effects were studied in [31].

Calculation of the change in the energy density of the ground state (first line in expression (14)) during the one-step transition from the energy scale to the scale gives the following result

Here, is the 5-dimensional volume. The result was obtained by combining expressions (B.4) and (B.5) in Appendix B.

Let us estimate the value of the total energy density shift provided that the energy scale is reduced from the initial scale to the scale where the fluctuations in the extra dimensions are suppressed. To this end, we use expression (24) to obtain inequalities were used here. The variation of mass was neglected due to its smallness proved above. The energy density can not be larger than the Planck one , hence the correction to the ground state energy density is small as compared to the initial value :

Evidently, such renormalization cannot make the -term be equal to the observational value which is almost zero.

#### 3. Moderate Energies: Reduction to 4 Dimensions

It was shown in the previous section that the physical parameters vary slowly with the energy, at least for the usual assumption on the coupling constant . Therefore, the shift of the parameter values from high energy to small energies is a serious problem. In this section, it will be shown that the extra dimensions supply us a more effective mechanism of parameters changing provided that the dimensionality of extra space . We will assume in this section.

There are five energy scalesâ€”the D-dimensional Planck mass , the initial energy scale where we intend to specify our Lagrangian, the scale which is related to a characteristic size of the compact extra dimensions, the electroweak scale where the parameter values are known, and the running scale .

Excitations discussed in the previous section act in each of dimensions if . The picture is simplified when the energy scale shifts below where the excitations of the extra space are suppressed, and hence, the extra metric is static. It is reasonable to integrate over the extra coordinates in this case. This strongly influences the values of the physical parameters as is discussed in this section.

Consider the scalar field action taken from (2) where . As was shown in [16, 32, 33], there exist static solution to the classical equation which are homogeneous in our 4-dim space. Let us decompose the field around its classical part where are the orthonormal eigen-functions of the dâ€™Alembert operator acting in the -dim extra space

Below, we limit ourselves by the only first term in the sum (29) so that

Here, is the volume of the compact extra space. This mode is distributed uniformly in the extra dimensions. After substitution (29) and (31) into expression (27), we get the following form of the effective 4-dim action for the scalar field where

Our aim is to reduce the effective mass in many orders of the magnitude provided that the initial mass . One could imagine that equation holds for a specific solution to equation (28) provided that . Indeed, numerical simulation indicates that an appropriate function can be found for a wide range of the coupling constant and the extra space volume . This means that we are able to substantially reduce the mass of the scalar field from the Planckian scale to the electroweak one. Moreover, its value at low energies could have any sign. The Higgs-like potential with two minima is realized if the sign of the mass term remains negative.

The cosmological constant is also a function of the classical field distribution in the extra dimensions. As was shown in [15], one can choose a function that gives zero value of the cosmological constant. Notice that so that a more complicated extra metric should be used in the future to simultaneously correct the mass and the Lambda term.

#### 4. Conclusion

In this paper, we use the Wilsonian approach to study the evolution of the physical parameter values defined at the sub-planckian energies to values at low energies. It is shown that all parameters are varied slowly as compared to their initial values which are of the order of the Planck scale. This means that we need an alternative mechanism that is responsible for a significant change in the parameter values so that they coincide with the observational ones. We study the role of the local extra dimensions in this relation.

The inclusion of the compact extra space has two consequences. The positive point is that the integration over extra dimensions is a promising way to substantially decrease the parameter values to be comparable with the observable values. At the same time, the integration over small energy layers which is intrinsic to the Wilsonian approach appears to be problematic due to the discreteness of the Kaluza-Klein energy levels. In this regard, the truncated Green functions were used for analysis.

It is also shown that for any mass of scalar field at low energies, there exists an inhomogeneous extra metric that relates this mass value to its value at the Planck energy scale.

The subject of this study relates to the Hierarchy problem which is widely discussed in the framework of the brane paradigm starting from the pioneering works [34, 35] where 4-dim manifolds (branes) attached to specific points of extra dimensions are postulated. Specific parameters of the branes are involved to succeed in the description of a variety phenomena [14]. Renormalization of the parameters is not considered usually. In our research, as was shown in [16], the brane could be formed due to the concentration of a scalar field which is governed by the classical equations of motion. It is the renormalization procedure in the presence of compact extra dimensions that plays the central role in this paper.

The integration over the extra dimensions looks a promising tool for a substantial shift of the parameter values to small ones at the low energy. A more general study based on the Green functions in the de Sitter metric [36] looks promising.

#### Appendix

#### A.1. A. Truncated Green Function in the Presence of the Compact Extra Dimensions

Here, we consider the integration of generating functional (13) over a finite set of modes of excitation in the space with metric . The case is considered as a specific example. The excitations are described by the eigen-functions of the Dâ€™Alembertian operator

The integration over a finite set of modes assumes the decomposition

Following the standard procedure for the calculation of generating functional (13), consider the solution to the equation

Comparison of expression (A.3) with the definition of the Green function gives the relation between the truncated Green function and the finite number of the eigen-functions

If is a full orthonormal set then represents the well-known form of the Green function.

Let us refine the formulas written above and apply them to our needs. The metric (4) leads to the decomposition which simplifies the expressions for the eigen-functions and eigen-values:

The form of excitations in the 4-dim Euclidean space is known as well as in the 1-dim extra space

Acting as in (18), the Green function (A.5) acquires the form

Summation over 4-dimensional excitations can be replaced by integration in a standard way with the result

To move ahead, we have to fix scales for the numerical estimations here and in the main text. Let , the extra space size is , and the primary energy scale is . Then, the number of extra space modes (or the Kaluza-Klein levels) is , and we may replace the sum over by the integral. Those part of the Green function that contains quick mode in 4-dim space (first line above) acquires the form

Here , and .

The second line in (A.13) is responsible for the only quick mode acting in the extra dimensions: and the truncated Green function at the energy level is as follows

#### A.2. B. Ground State Energy in the Presence of the Compact Extra Dimensions

The shift of the ground state energy (the first exponent in (14)) is represented in this Appendix. The contribution of layers in the interval from (17) is as follows

The first term in the sum represents the contribution of the quick modes in the 4-dim space. The last term includes all modes in the 4-dim spaceâ€”quick and slowâ€”and quick excitation with the number acting in the extra dimensions. All these excitations are characterized by wavelength in the interval in 4 dimensions or in the extra space. The sums over and can be converted into the integral in the standard form and we get the Euclidean version of the energy density

Here, and is the 5-dimensional volume. is 4-dim volume in the Euclidean space. The interval of the energy layer is assumed to be small, and we neglect variation of the physical parameters within this interval. Then, (B.2) is where .

Remind that we are integrating over the wavelength interval . Let us express everything in terms of the left edge of the interval or the wave number . The wavelength of the scalar field excitation in extra space is . Hence, .

The right edge of the interval is defined as follows: that leads to the interval and ()

According to the discussion made in Appendix A, the sum in (B.4) can be approximated by the integral

Finally, (B.4) is transformed in the following form

#### Data Availability

The data used to support the findings of this study are included within the article in the form of bibliography references.

#### Conflicts of Interest

The author declares that they have no conflicts of interest.

#### Acknowledgments

The work was supported by the Ministry of Science and Higher Education of the Russian Federation, Project â€śFundamental properties of elementary particles and cosmologyâ€ť no. 0723-2020-0041 and according to the Russian Government Program of Competitive Growth of Kazan Federal University.

#### References

- A. Loeb, â€śAn observational test for the anthropic origin of the cosmological constant,â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2006, no. 5, p. 009, 2006. View at: Publisher Site | Google Scholar - A. Ashoorioon, K. Dimopoulos, M. M. Sheikh-Jabbari, and G. Shiu, â€śReconciliation of high energy scale models of inflation with Planck,â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2014, no. 2, p. 025, 2014. View at: Publisher Site | Google Scholar - H. Robert, A. N. Brandenberger, S. P. Patil, and C. Vafa, â€śString gas cosmology and structure formation,â€ť
*International Journal of Modern Physics A: Particles and Fields; Gravitation; Cosmology; Nuclear Physics*, vol. 22, pp. 3621â€“3642, 2012. View at: Publisher Site | Google Scholar - M. Tegmark, A. Aguirre, M. Rees, and F. Wilczek, â€śDimensionless constants, cosmology and other dark matters,â€ť
*Physics Review D*, vol. 73, no. 2, article 023505, 2006. View at: Publisher Site | Google Scholar - M. Chaichian and A. B. Kobakhidze, â€śMass hierarchy and localization of gravity in extra time,â€ť
*Physics Letters B*, vol. 488, no. 2, pp. 117â€“122, 2000. View at: Publisher Site | Google Scholar - M. P. Hertzberg and A. Masoumi, â€śCan compactifications solve the cosmological constant problem?â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2016, no. 6, p. 053, 2016. View at: Publisher Site | Google Scholar - A. Babic, B. Guberina, R. Horvat, and H. Stefancic, â€śRenormalization group running of the cosmological constant and its implication for the Higgs boson mass in the standard model,â€ť
*Physics Review D*, vol. 65, no. 8, article 085002, 2002. View at: Publisher Site | Google Scholar - E. Dudas, C. Papineau, and V. A. Rubakov, â€śFlowing to four dimensions,â€ť
*Journal of High Energy Physics*, vol. 2006, no. 3, p. 085, 2006. View at: Publisher Site | Google Scholar - C. P. Burgess, â€śThe Cosmological Constant Problem: Why itâ€™s hard to get Dark Energy from Micro-physics,â€ť in
*Proceedings, 100th Les Houches Summer School: Post-Planck Cosmology*, pp. 149â€“197, Les Houches, France, July-August 2013. View at: Google Scholar - C. Ringeval, T. Suyama, and M. Yamaguchi, â€śLarge mass hierarchy from a small nonminimal coupling,â€ť
*Physical Review D*, vol. 99, no. 12, 2019. View at: Publisher Site | Google Scholar - N. Arkani-Hamed, S. Dimopoulos, and G. R. Dvali, â€śThe hierarchy problem and new dimensions at a millimeter,â€ť
*Physics Letters B*, vol. 429, no. 3-4, pp. 263â€“272, 1998. View at: Publisher Site | Google Scholar - B. Guo, Y.-X. Liu, K. Yang, and S.-W. Wei, â€śHierarchy problem and new warped extra dimension,â€ť
*Physics Review D*, vol. 98, no. 8, article 085022, 2018. View at: Publisher Site | Google Scholar - L. Randall and R. Sundrum, â€śLarge mass hierarchy from a small extra dimension,â€ť
*Physical Review Letters*, vol. 83, no. 17, pp. 3370â€“3373, 1999. View at: Publisher Site | Google Scholar - M. Shifman, â€śLarge extra dimensions: becoming acquainted with an alternative paradigm,â€ť
*International Journal of Modern Physics A: Particles and Fields; Gravitation; Cosmology; Nuclear Physics*, vol. 25, pp. 199â€“225, 2012. View at: Google Scholar - S. G. Rubin, â€śInhomogeneous extra space as a tool for the top-down approach,â€ť
*Advances in High Energy Physics*, vol. 2018, Article ID 2767410, 8 pages, 2018. View at: Publisher Site | Google Scholar - S. G. Rubin, â€śScalar field localization on deformed extra space,â€ť
*The European Physical Journal C*, vol. 75, no. 7, p. 333, 2015. View at: Publisher Site | Google Scholar - I. G. Marian, N. Defenu, U. D. Jentschura, A. Trombettoni, and I. Nandori, â€śRenormalization-group running induced cosmic inflation,â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2020, no. 6, 2020. View at: Publisher Site | Google Scholar - S. Nojiri, S. D. Odintsov, and V. K. Oikonomou, â€śModified gravity theories on a nutshell: inflation, bounce and late-time evolution,â€ť
*Physics Reports*, vol. 692, pp. 1â€“104, 2017. View at: Publisher Site | Google Scholar - A. De Felice and S. Tsujikawa, â€śf(R) theories,â€ť
*Living Reviews in Relativity*, vol. 13, no. 1, 2010. View at: Publisher Site | Google Scholar - A. A. Starobinsky, â€śSpectrum of relict gravitational radiation and the early state of the universe,â€ť
*Journal of Experimental and Theoretical Physics Letters*, vol. 30, p. 682, 1979. View at: Google Scholar - A. A. Starobinsky, â€śA new type of isotropic cosmological models without singularity,â€ť
*Physics Letters B*, vol. 91, no. 1, pp. 99â€“102, 1980. View at: Publisher Site | Google Scholar - K. Bamba, A. N. Makarenko, A. N. Myagky, S. Nojiri, and S. D. Odintsov, â€śBounce cosmology from F(R) gravity and F(R) bigravity,â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2014, no. 1, p. 8, 2014. View at: Publisher Site | Google Scholar - A. A. Starobinsky, S. V. Sushkov, and M. S. Volkov, â€śAnisotropy screening in horndeski cosmologies,â€ť
*Physical Review D*, vol. 101, no. 6, 2020. View at: Publisher Site | Google Scholar - Y. Lyakhova, A. A. Popov, and S. G. Rubin, â€śClassical evolution of subspaces,â€ť
*European Physical Journal C: Particles and Fields*, vol. 78, no. 9, p. 764, 2018. View at: Publisher Site | Google Scholar - J. C. Fabris, A. A. Popov, and S. G. Rubin, â€śMultidimensional gravity with higher derivatives and inflation,â€ť
*Physics Letters B*, vol. 806, article 135458, 2020. View at: Publisher Site | Google Scholar - F. Bezrukov and M. Shaposhnikov, â€śThe Standard Model Higgs boson as the inflaton,â€ť
*Physics Letters B*, vol. 659, no. 3, pp. 703â€“706, 2008. View at: Publisher Site | Google Scholar - A. D. Linde,
*Particle Physics and in Ationary Cosmology*, Harwood Academic Publishers, Switzerland, 1990. - M. E. Peskin and D. V. Schroeder,
*An Introduction to Quantum Eld Theory*, 1995. - J. M. Overduin and P. S. Wesson, â€śKaluza-Klein gravity,â€ť
*Physics Reports*, vol. 283, no. 5-6, pp. 303â€“378, 1997. View at: Publisher Site | Google Scholar - D. Ashok, â€śField theory,â€ť in
*A Path Integral Approach*, World Scientific Publishing Company Pte Limited, 3rd edition, 2019. View at: Google Scholar - S. Bauman and K. R. Dienes, â€śKaluza-klein masses and couplings: radiative corrections to tree-level relations,â€ť
*Physical Review D*, vol. 85, no. 12, 2012. View at: Publisher Site | Google Scholar - V. A. Gani, A. E. Dmitriev, and S. G. Rubin, â€śDeformed compact extra space as dark matter candidate,â€ť
*International Journal of Modern Physics D: Gravitation; Astrophysics and Cosmology*, vol. 24, article 1545001, 2015. View at: Google Scholar - K. A. Bronnikov, R. I. Budaev, A. V. Grobov, A. E. Dmitriev, and S. G. Rubin, â€śInhomogeneous compact extra dimensions,â€ť
*Journal of Cosmology and Astroparticle Physics*, vol. 2017, no. 10, p. 001, 2017. View at: Publisher Site | Google Scholar - M. Gogberashvili, â€śOur world as an expanding shell,â€ť
*Europhysics Letters*, vol. 49, no. 3, pp. 396â€“399, 2000. View at: Publisher Site | Google Scholar - L. Randall and R. Sundrum, â€śAn alternative to Compactification,â€ť
*Physical Review Letters*, vol. 83, no. 23, pp. 4690â€“4693, 1999. View at: Publisher Site | Google Scholar - E. T. Akhmedov, K. V. Bazarov, D. V. Diakonov, U. Moschella, F. K. Popov, and C. Schubert, â€śPropagators and Gaussian effective actions in various patches of de sitter space,â€ť
*Physics Review D*, vol. 100, no. 10, article 105011, 2019. View at: Publisher Site | Google Scholar

#### Copyright

Copyright © 2020 Sergey G. Rubin. 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.