Research Article | Open Access

# Testing a Dilaton Gravity Model Using Nucleosynthesis

**Academic Editor:**Elias C. Vagenas

#### Abstract

Big bang nucleosynthesis (BBN) offers one of the most strict evidences for the -CDM cosmology at present, as well as the cosmic microwave background (CMB) radiation. In this work, our main aim is to present the outcomes of our calculations related to primordial abundances of light elements, in the context of higher dimensional steady-state universe model in the dilaton gravity. Our results show that abundances of light elements (primordial D, ^{3}He, ^{4}He, T, and ^{7}Li) are significantly different for some cases, and a comparison is given between a particular dilaton gravity model and -CDM in the light of the astrophysical observations.

#### 1. Introduction

The current expansion of the universe is a crucial evidence for the big bang cosmology model. It predicts the chemical abundances of primordial elements as a result of nuclear reactions which began seconds after the big bang and continued for the next several minutes. With the help of inflation, one can consistently solve the well-known problems of the standard model, such as the observed spatial homogeneity, isotropy, and flatness of the universe [1].

There are still many unsolved puzzles of this model, such as the origin of dark matter and dark energy, cosmological constant problem, cosmic coincidence problem, and the exact form of the inflation potential [2, 3]. On the other hand, there are many models which claim solutions to these problems by modifying Einstein’s general relativity. Quintessence, -essence, phantom, quintom, and other phenomenological models are just few examples of alternate gravity models that offer a solution to the dark energy problem [4]. And also there are alternative gravity theories that suggest using extra fields (scalar tensor, etc.) and higher dimensions (Kaluze-Klein, Randall-Sundrum) arising from string theory at the low-energy limit [5].

In this ocean of models, we would like to consider an observable consequence (modified abundances of light elements) of a new model, a higher dimensional dilaton gravity theory of steady-state cosmological (HDGS) model in the context of string theory. We need to highlight that the original steady-state model [6, 7] is unfavorable compared to the standard big bang scenario. But our motivation in this work is to suggest a test of a specific higher dimensional dilaton gravity model which effectively mimics the standard FRW model with the modified Hubble constant. Hence, an immediate consequence would be the modification of nucleosynthesis.

This modification was investigated in [8] and it was claimed that this model gives a better estimate for the primordial ^{4}He abundance compared to the standard big bang nucleosynthesis (SBBN) by choosing the number of dimensions appropriately. In this work, to further test their strong claim, we calculated the abundances of the primordial D, ^{3}He, ^{4}He, T, and ^{7}Li in the context of this nonstandard (HDGS) model and compared it with the predictions of SBBN and the astrophysical observations.

On the other hand, at high energies, the quantum gravitational corrections will start to play an important role. Quantum corrections will modify the dilaton gravity models as well and therefore change the whole form of this model via action [9–12]. One would naturally expect to see quantum effects during the very early universe such as primordial inflationary stage. During inflation, quantum loop effects may lead to very small [13, 14] but possibly observable corrections to power spectrum [15–20]. Therefore, one might describe the interactions with effective field theories of inflation [21]. But, in this work, we are mainly interested in the consequence of a geometrical constraint: -dimensional universe having a constant volume, leading to a modified Hubble parameter during a later stage, nucleosynthesis, where quantum gravitational corrections are negligible.

The paper is organized as follows. In Section 2, dynamics of this particular dilaton gravity model is summarized. In Section 3, nucleosynthesis in the context of this model is analyzed. In Section 4, the results obtained from our calculations for this model and the predictions of SBBN with the help of Planck satellite data [22] are compared with the astrophysical observations.

#### 2. Dynamics of HDGS: A Dilaton Gravity Model

In this section, we briefly summarize the dynamics of a particular type of dilaton gravity models proposed in [8]. The idea is introducing a higher dimensional dilaton gravity action of steady-state cosmology (HDGS) in the string frame. Therefore, the evolution of the internal -dimensional space results in an evolution of the observed universe to keep the whole system in a steady state. Due to this constraint, choosing particular values, for some parameters, such as the number of extra dimensions, leads to possibly observable effects in our universe. Let us start with the action, which stems from the low-energy effective string theory, where is the curvature scalar, stands for manifold, corresponds to extra dimensions, is the determinant of metric tensor, is the dilaton field taken as space independent real function of time, and is an arbitrary coupling constant. is a real smooth function of the dilaton field and corresponds to the dilaton self-interaction potential and both and are real parameters. Two interesting cases that are worth mentioning are and , corresponding to anomaly-free superstring theory and with corresponds to bosonic string theory. The metric is given by Here, is the cosmic time and are the cartesian coordinates of the 3-dimensional flat space, basically the observed universe. The coordinates, , are -dimensional, compact (torodial) internal space coordinates (this represents space that cannot be observed directly and locally today). While denotes the scale factor of 3-dimensional external space, is the scale factor of -dimensional internal space.

This model has the following key properties.

(i) The -dimensional universe has a constant volume; that is, , hence steady state. But the internal and external spaces are dynamical. (ii) The energy density is constant in the higher dimensional universe. (iii) There is no higher dimensional matter source other than the dilaton field in the action.

If the scalar field is redefined as , the relation between the scalar field and the scale factor of the external space turns out to be where is a constant of integration. Here, prime denotes derivative with respect to the ordinary time. Imposing the constant volume condition gives where and correspond to the integration constants. Therefore, the modified Hubble parameter of the external space is obtained as follows: Here, the physically relevant case is the solution for expanding external space with . The deceleration parameter for the external space is given by In the case of and , and with the choice of appropriate initial conditions, it turns out that [8] the early time modified deceleration parameter is given by

#### 3. Nucleosynthesis in HDGS

We are interested in how abundances of light elements would change in the context of this model. Specifically, we would like to consider the ratio of the modified expansion rate to the standard expansion rate during the early radiation dominant epoch. This ratio is given by This is true, since deceleration parameter stays almost constant during primordial nucleosynthesis. The value of the deceleration parameter for standard BBN is . Since is given by (7), the so-called standard expansion factor, , can be expressed in terms of and as

If is taken, it denotes nonstandard expansion factor. This kind of modification might also arise due to additional light particles such as neutrinos which would make the ratio be . In this context of the dilaton gravity model that we mentioned, it is also going to occur due to a modification of general relativity. We are interested in the case where and therefore the value of will come only from the modification of general relativity.

The primordial abundances of the light elements (primordial D, ^{3}He, ^{4}He, ^{7}Li, and T) depend on the baryon density and the expansion rate of the universe [23, 24]. The baryon density parameter [23] is given by
where gives the baryon to photon ratio, is dimensionless current critical cosmological density parameter for baryons, and with being the present value of the Hubble parameter. Any modification of the expansion rate would change the time when neutrons freeze out, which will in turn determine the final abundance of helium-4 as well as all of the other light elements.

In the following subsections, we will analyze nucleosynthesis due to a modification of the expansion rate in the context of HDGS models. We will express the primordial nuclear abundances of light nuclei in terms of two parameters of HDGS models: number of extra dimensions and coupling constant . Particularly, we will be interested in the case of , where and correspond to anomaly-free superstring and bosonic string theory, respectively.

##### 3.1. ^{4}He Abundance in HDGS Models

The two body reaction chains of light elements, which include deuterium (D), tritium (T), and helium-3 (^{3}He) to produce helium-4 (^{4}He), are more efficient than four body reactions of neutrons and protons. The first step is producing D from . After that, D is converted into ^{3}He and T as follows:
and, finally, ^{4}He is produced from D combining with T and ^{3}He

In order to get precise estimates for abundances of light elements, one should solve nonlinear differential equations of the nuclear reaction network. This problem can be studied numerically and the modern methods are based on Wagoner et al. [25] code and its updated version by Smith et al. [26]. The next step is getting a best fit to a numerical work to see how various abundances depend on and other parameters such as number of extra neutrinos. Another venue is applying semianalytical methods, where one of the earliest works was done by Esmailzadeh et al. [27] using the method of fixed points.

In this work, we would like to use, if there exists, the best fit expressions for certain elements. If there is none in the literature for a certain element, then we will use a semianalytical approach that is based on a simple assumption, which is the nuclear reaction network obeying in a quasiequilibrium state. In this state, basically one assumes that “the total flux coming into each corresponding reservoir must be equal to the outgoing flux” [28].

A simple way of estimating of ^{4}He abundance (in general, abundance by weight is related to the ratio of number density of a particular element to the number density of all nucleons (including the ones in complex nuclei), , where is the mass number of a particular element; e.g., for helium) is the following: multiply the abundance of neutrons by two at the time when the deuterium bottleneck opens up. Here, we will refer to the best fit expression for ^{4}He abundance that includes the case of modified expansion rate [29, 30]:
where stands for the primordial abundance. We will take [31] from here on. The SBBN value, , becomes . Using (9), for the case of HDGS models that we are interested in, one can get the following expression for ^{4}He abundance in terms of and as [8]
In the case of , the predicted values are obtained as and , for and , respectively.

From the observational point of view, the ^{4}He primordial abundance, , is determined from the recombination of lines of the H II from blue compact galaxies (BCGs) [32]. The observational results of the ^{4}He abundances are given by [33] and [34].

##### 3.2. Abundances of Other Light Elements in HDGS Models

###### 3.2.1. Deuterium Abundance

Deuterium is produced by and used in four types of reactions (11), (12). Therefore, one would expect to solve either numerically or analytically the equations for this nuclear reaction network and get the expression for deuterium abundance, , where and are the number densities of deuterium and all nucleons, respectively.

In literature, instead of abundances of elements, their abundances relative to hydrogen are given. To see why, let us look at how deuterium is determined. The absorbed primordial element has more space in the wings of the observed quasar absorption-line systems (QAS) [35–39] than the absorbed hydrogen at high redshifts (z) and/or at low metallicity (Z). Also, the observation of the multicomponent velocities of these absorbed elements is very significant in order to determine the abundance of deuterium. Therefore, the ratio is more meaningful and is often known as interstellar medium measurement for deuterium abundance. This ratio can be expressed in terms of the abundance by weight of the deuterium as The factor, , comes from the fact that mass number of deuterium is 2 and hydrogen number density is equal to of all the nucleons in the universe, that is, 75% by weight.

Let us start with the semianalytical expression for the abundance of deuterium to calculate (15). Using the quasiequilibrium condition, one can get [28] where [28], , and . Here, the coefficients and are related to experimental values of nuclear reaction rates of deuterium at temperature of order 0.08 MeV. (We assume that the nuclear interaction rates are independent of extra dimensions. We also assume that there are no matter sources in higher dimensions and HDGS is a Kaluza-Klein-type model rather than a brane world cosmology one.) Putting this value in (15) gives .

Let us now use a more precise expression for deuterium abundance [23] based on a numerical best fit: From this expression, one can get the SBBN value of (for and ) as . Comparing this number with the one from the semianalytical method, , we can safely assume a quasiequilibrium condition, if necessary.

By using (9), one can express for HDGS models as Taking , the predicted values of are obtained as and for and , respectively, for model.

Finally, the observational results are [40] and [39].

###### 3.2.2. Helium-3 Abundance

The relevant nuclear reactions that involve ^{3}He are

The quantity used in the literature to describe ^{3}He is
Making a quasiequilibrium approximation for ^{3}He abundance, we can express the ^{3}He abundance in terms of deuterium abundance after using the experimental values for the ratios of the related nuclear reaction rates [28]
From this equation, we can see that ^{3}He abundance is not as sensitive as deuterium since a change in deuterium abundance would change both parts of the ratio. One can also see this from the weaker dependence of on , compared to , for SBBN best fit expression [41]. Consider
Therefore, ^{3}He abundance is not a good indicator of a modification of SBBN due to HDGS models.

###### 3.2.3. Tritium Abundance

Using the quasiequilibrium condition for tritium, [28] is obtained as It is clear from this expression that the value of tritium abundance will be as sensitive as deuterium abundance to any modification of the expansion rate. But the magnitude of tritium abundance is two orders of magnitude smaller than both deuterium and helium-3. Therefore, observationally, it is not very feasible, but it should be kept in mind that it can be used to test for consistency in the future experiments.

###### 3.2.4. Lithium-7 Abundance

Finally, we would like to investigate the effects of modified expansion rate on lithium abundance. The Li abundance is given by One might think that its smallness would make it irrelevant for observational purposes. But it can actually be measured in the atmospheres of metal-poor stars in the stellar halo of Milky Way. All primordial elements point towards the same parameter except lithium. The ratio of the expected SBBN value of lithium-7 abundance to the observed one is between 2.4 and 4.3 [42]. Therefore, it should be interesting to check if these HDGS models offer any solution to the lithium problem.

The best fit expression to the numerical BBN data of the is given in [23] as Taking and , the SBBN value of lithium-7 abundance is found as . In terms of and , the modified form of (25) becomes By using (26), the predicted values are found as for and for , for the case of .

#### 4. Discussion

We have shown in this work that one gets a considerable modification to the primordial abundances of light elements in the case of a higher dimensional steady-state universe in dilaton gravity (there are other ways to modify BBN based on scalar-tensor theories; for details, see [45–47] and references therein.). Although there is a huge class of models that one can consider, with two free parameters (dilaton coupling constant) and (number of internal dimensions). Here we focused on two interesting cases: with (anomaly-free superstring theory), and with (bosonic string theory).

The main idea behind the calculation is modifying the expansion rate during the nucleosynthesis to get different abundances for light elements. One can think of the modification as being similar to adding more relativistic particles, such as extra neutrinos, into the standard big bang model. When Hubble parameter gets modified, all the nucleosynthesis will get modified as well. The question is the following: is this modification large enough to observe and if it is then is it compatible with the data?

To answer these questions, one should analyze how the nuclear reactions get modified with the modification of the expansion rate. It is well-known that the complete analysis of the nuclear reactions governing the primordial abundances of light elements can be done using numerical methods. We used the results of the previous works, where we can, which were obtained by getting best fit expressions to numerical data related to the abundances of these elements. And if there are no known best fit expressions in the literature, we proceeded our analysis based on semianalytical methods.

The primordial abundance of helium-4 was already studied in the context of these models. It was pointed out that case is more compatible with helium-4 data compared to the standard big bang scenario. We made a more extensive analysis of other light elements and checked the compatibility of this model with astrophysical observables. The results are summarized in Table 1.

One can clearly see from Table 1 that and dilaton gravity model is incompatible with helium-4 data and is incompatible with deuterium as well. Helium-4 data favoured the case of and compared to SBBN, as was noted. In the case of deuterium, earlier measurements favour (with almost being inside the error bars) dilaton gravity model whereas the more recent measurements rule them out and point towards SBBN. Therefore, it is fair to say that one needs more observations and data analysis to see which model is favoured.

We also showed that helium-3 and tritium abundances are not very convenient to see a modification of the standard model in the context of the dilaton gravity model considered here. And for the case of lithium-7 one gets almost a ten percent decrease for the expected abundance, compared to SBBN, but it is still far from explaining the observed abundance. So, these models do not offer a solution to the* lithium problem*; therefore, the existence of this problem still preserves its place in the literature and leaves an open window to new physics.

#### Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

#### Acknowledgments

The authors would like to thank Özgür Akarsu, Ali Kaya, and Subir Sarkar for the helpful discussions. This work was supported by TÜBİTAK-1001 Grant no. 112T817.

#### References

- A. Linde, “Inflationary cosmology,” in
*Inflationary Cosmology*, vol. 738 of*Lecture Notes in Physics*, pp. 1–54, 2007. View at: Publisher Site | Google Scholar - P. J. E. Peebles and B. Ratra, “The cosmological constant and dark energy,”
*Reviews of Modern Physics*, vol. 75, no. 2, pp. 559–606, 2003. View at: Publisher Site | Google Scholar | Zentralblatt MATH | MathSciNet - S. Perlmutter, G. Aldering, G. Goldhaber et al., “Measurements of Ω and Λ from 42 high-redshift supernovae,”
*The Astrophysical Journal*, vol. 517, no. 2, pp. 565–586, 1999. View at: Publisher Site | Google Scholar - R. Durrer and R. Maartens, “Dark energy and modified gravity,” in
*Dark Energy: Observational and Theoretical Approaches*, P. Ruiz-Lapuente, Ed., pp. 48–91, Cambridge University Press, 2010. View at: Google Scholar - L. Randall and R. Sundrum, “Large mass hierarchy from a small extra dimension,”
*Physical Review Letters*, vol. 83, no. 17, pp. 3370–3373, 1999. View at: Publisher Site | Google Scholar | Zentralblatt MATH | MathSciNet - H. Bondi and T. Gold, “The steady-state theory of the expanding Universe,”
*Monthly Notices of the Royal Astronomical Society*, vol. 108, no. 3, pp. 252–270, 1948. View at: Google Scholar - F. Hoyle, “A new model for the expanding universe,”
*Monthly Notices of the Royal Astronomical Society*, vol. 108, pp. 372–382, 1948. View at: Google Scholar - Ö. Akarsu and T. Dereli, “Late time acceleration of the 3-space in a higher dimensional steady state universe in dilaton gravity,”
*Journal of Cosmology and Astroparticle Physics*, vol. 2013, no. 2, article 050, 2013. View at: Publisher Site | Google Scholar - S. Nojiri, O. Obregon, and S. D. Odintsov, “(Non)-singular brane-world cosmology induced by quantum effects in five-dimensional dilatonic gravity,”
*Physical Review D*, vol. 62, Article ID 104003, 2000. View at: Publisher Site | Google Scholar - S. Nojiri and S. D. Odintsov, “Quantum dilatonic gravity in d = 2,4 and 5 dimensions,”
*International Journal of Modern Physics A*, vol. 16, no. 6, pp. 1015–1108, 2001. View at: Publisher Site | Google Scholar - S. Nojiri and S. D. Odintsov, “Introduction to modified gravity and gravitational alternative for dark energy,”
*International Journal of Geometric Methods in Modern Physics*, vol. 4, no. 1, pp. 115–145, 2007. View at: Publisher Site | Google Scholar | MathSciNet - E. Elizalde, S. Jhingan, S. Nojiri, S. D. Odintsov, M. Sami, and I. Thongkool, “Dark energy generated from a (super-) string effective action with higher-order curvature corrections and a dynamical dilaton,”
*The European Physical Journal C*, vol. 53, no. 3, pp. 447–457, 2008. View at: Publisher Site | Google Scholar - S. Wienberg, “Quantum contributions to cosmological correlations,”
*Physical Review D*, vol. 72, no. 4, Article ID 043514, 19 pages, 2005. View at: Google Scholar - S. Weinberg, “Quantum contributions to cosmological correlations. II. Can these corrections become large?”
*Physical Review D*, vol. 74, Article ID 023508, 2006. View at: Publisher Site | Google Scholar - D. Seery, “One-loop corrections to a scalar field during inflation,”
*Journal of Cosmology and Astroparticle Physics*, vol. 711, p. 25, 2007. View at: Google Scholar - D. Seery, “One-loop corrections to the curvature perturbation from inflation,”
*Journal of Cosmology and Astroparticle Physics*, vol. 2008, p. 006, 2008. View at: Publisher Site | Google Scholar - D. Marolf and I. A. Morrison, “Infrared stability of de Sitter space: loop corrections to scalar propagators,”
*Physical Review D*, vol. 82, Article ID 105032, 2010. View at: Publisher Site | Google Scholar - S. B. Giddings and M. S. Sloth, “Semiclassical relations and IR effects in de Sitter and slow-roll space-times,”
*Journal of Cosmology and Astroparticle Physics*, vol. 1101, article 023, 2011. View at: Publisher Site | Google Scholar - E. O. Kahya and V. K. Onemli, “Quantum stability of a
*w*< −1 phase of cosmic acceleration,”*Physical Review D*, vol. 76, Article ID 043512, 2007. View at: Google Scholar - E. O. Kahya and R. P. Woodard, “Scalar field equations from quantum gravity during inflation,”
*Physical Review D: Particles, Fields, Gravitation, and Cosmology*, vol. 77, no. 8, 2008. View at: Publisher Site | Google Scholar | MathSciNet - C. Cheung, P. Creminelli, A. L. Fitzpatrick, J. Kaplan, and L. Senatore, “The effective field theory of inflation,”
*Journal of High Energy Physics*, vol. 2008, no. 3, article 014, 2008. View at: Google Scholar - P. A. R. Ade, N. Aghanim, C. Armitage-Caplan et al., “Planck 2013 results—XVI. Cosmological parameters,” http://arxiv.org/abs/1303.5076. View at: Google Scholar
- G. Steigman, “Neutrinos and big bang nucleosynthesis,”
*Advances in High Energy Physics*, vol. 2012, Article ID 268321, 24 pages, 2012. View at: Publisher Site | Google Scholar - V. Simha and G. Steigman, “Constraining the early-Universe baryon density and expansion rate,”
*Journal of Cosmology and Astroparticle Physics*, vol. 2008, no. 6, article 16, 2008. View at: Google Scholar - R. V. Wagoner, W. A. Fowler, and F. Hoyle, “On the synthesis of elements at very high temperatures,”
*The Astrophysical Journal*, vol. 148, p. 3, 1967. View at: Publisher Site | Google Scholar - M. S. Smith, L. H. Kawano, and R. A. Malaney, “Experimental, computational, and observational analysis of primordial nucleosynthesis,”
*The Astrophysical Journal, Supplement Series*, vol. 85, no. 2, pp. 219–247, 1993. View at: Publisher Site | Google Scholar - R. Esmailzadeh, G. D. Starkman, and S. Dimopoulos, “Primordial nucleosynthesis without a computer,”
*Astrophysical Journal Letters*, vol. 378, no. 2, pp. 504–518, 1991. View at: Publisher Site | Google Scholar - V. Mukhanov,
*The Physical Foundation of Cosmology*, Cambridge University Press, Cambridge, Mass, USA, 2005. - J. P. Kneller and G. Steigman, “BBN for pedestrians,”
*New Journal of Physics*, vol. 6, article 117, 2004. View at: Publisher Site | Google Scholar - G. Steigman, “Primordial nucleosynthesis in the precision cosmology era,”
*Annual Review of Nuclear and Particle Science*, vol. 57, pp. 463–491, 2007. View at: Publisher Site | Google Scholar - E. Komatsu, K. M. Smith, J. Dunkley (WMAP Collaboration) et al., “Seven-year Wilkinson microwave anisotropy probe (WMAP
^{∗}) observations: cosmological interpretation,”*The Astrophysical Journal Supplement Series*, vol. 192, no. 2, article 18, 2011. View at: Publisher Site | Google Scholar - B. E. J. Pagel, E. A. Simonson, R. J. Terlevich, and M. G. Edmunds, “The primordial helium abundance from observations of extragalactic HII regions,”
*Monthly Notices of the Royal Astronomical Society*, vol. 255, pp. 325–345, 1992. View at: Google Scholar - Y. I. Izotov and T. X. Thuan, “The primordial abundance of 4He: evidence for non-standard big bang nucleosynthesis,”
*Astrophysical Journal Letters*, vol. 710, no. 1, pp. L67–L71, 2010. View at: Publisher Site | Google Scholar - E. Aver, K. A. Olive, and E. D. Skillman, “A new approach to systematic uncertainties and self-consistency in helium abundance determinations,”
*Journal of Cosmology and Astroparticle Physics*, vol. 2010, no. 5, article 3, 2010. View at: Publisher Site | Google Scholar - D. Kirkman, D. Tytler, N. Suzuki, J. M. O'Meara, and D. Lubin, “The cosmological baryon density from the deuterium-to-hydrogen ratio in QSO absorption systems: D/H toward Q1243+3047,”
*The Astrophysical Journal, Supplement Series*, vol. 149, no. 1, pp. 1–28, 2003. View at: Publisher Site | Google Scholar - J. M. O'Meara, S. Burles, J. X. Prochaska, G. E. Prochter, R. A. Bernstein, and K. M. Burgess, “The deuterium-to-hydrogen abundance ratio toward the QSO SDSS J155810.16-003120.0 1,”
*Astrophysical Journal Letters*, vol. 649, no. 2, pp. L61–L65, 2006. View at: Publisher Site | Google Scholar - M. Pettini, B. J. Zych, M. T. Murphy, A. Lewis, and C. C. Steidel, “Deuterium abundance in the most metal-poor damped Lyman alpha system: converging on $\mathrm{\Omega}$
_{b},_{0}*h*^{2},”*Monthly Notices of the Royal Astronomical Society*, vol. 391, no. 4, pp. 1499–1510, 2008. View at: Publisher Site | Google Scholar - M. Fumagalli, J. M. O'Meara, and J. X. Prochaska, “Detection of pristine gas two billion years after the big bang,”
*Science*, vol. 334, no. 6060, pp. 1245–1249, 2011. View at: Publisher Site | Google Scholar - M. Pettini and R. Cooke, “A new, precise measurement of the primordial abundance of Deuterium,” http://arxiv.org/pdf/1205.3785.pdf. View at: Google Scholar
- F. Iocco, G. Mangano, G. Miele, O. Pisanti, and P. D. Serpico, “Primordial nucleosynthesis: from precision cosmology to fundamental physics,”
*Physics Reports*, vol. 472, no. 1–6, pp. 1–76, 2009. View at: Publisher Site | Google Scholar - G. Steigman, “Primordial nucleosynthesis: successes and challenges,”
*International Journal of Modern Physics E*, vol. 15, no. 1, pp. 1–36, 2006. View at: Publisher Site | Google Scholar - B. D. Fields, “The primordial lithium problem,”
*Annual Review of Nuclear and Particle Science*, vol. 61, pp. 47–68, 2011. View at: Publisher Site | Google Scholar - M. Asplund, D. L. Lambertm, P. E. Nissen et al., “Lithium isotopic abundances in metal-poor halo stars,”
*The Astrophysical Journal*, vol. 644, p. 229, 2006. View at: Publisher Site | Google Scholar - S. G. Ryan, T. C. Beers, K. A. Olive, B. D. Fields, and J. E. Norris, “Primordial lithium and big bang nucleosynthesis,”
*The Astrophysical Journal Letters*, vol. 530, pp. L57–L60, 2000. View at: Google Scholar - T. Damour and B. Pichon, “Big bang nucleosynthesis and tensor-scalar gravity,”
*Physical Review D*, vol. 59, Article ID 123502, 1999. View at: Publisher Site | Google Scholar - A. Coc, K. A. Olive, J. P. Uzan, and E. Vangioni, “Big bang nucleosynthesis constraints on scalar-tensor theories of gravity,”
*Physical Review D*, vol. 73, Article ID 083525, 2006. View at: Publisher Site | Google Scholar - J. A. R. Cembranos, K. A. Olive, M. Peloso, and J.-P. Uzan, “Quantum corrections to the cosmological evolution of conformally coupled fields,”
*Journal of Cosmology and Astroparticle Physics*, vol. 907, article 025, 2009. View at: Publisher Site | Google Scholar

#### Copyright

Copyright © 2014 S. Boran and E. O. Kahya. 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}.