SciELO - Scientific Electronic Library Online

vol.62 issue3Density of modes maps for design of photonic crystal devicesDissociation-ionization and ionization-dissociation by multiphoton absorption of acetaldehyde at 266 and 355 nm. Dissociation pathways author indexsubject indexsearch form
Home Pagealphabetic serial listing  

Services on Demand




Related links

  • Have no similar articlesSimilars in SciELO


Revista mexicana de física

Print version ISSN 0035-001X

Rev. mex. fis. vol.62 n.3 México May./Jun. 2016



Gravitational collapse in brane-worlds revisited

M.A. García-Aspeitiaa  b 

C. Ortizb 

J.C. López-Domínguezb 

S. Hinojosa-Ruizb 

M.J. Reyes-Ibarrac 

aConsejo Nacional de Ciencia y Tecnología, Av., Insurgentes Sur 1582. Colonia Crédito Constructor, Del. Benito Juárez, 03940, México D.F. México.

bUnidad Académica de Física, Universidad Autónoma de Zacatecas, Calzada Solidaridad esquina con Paseo a la Bufa S/N, 98060, Zacatecas, México,

cDepartamento de Física, Centro de Investigación y de Estudios Avanzados del Instituto Politécnico Nacional, 2508, San Pedro Zacatenco, 07360, Gustavo A. Madero, Ciudad de México, México.


This paper is dedicated to revisit the modifications caused by branes in the collapse of a stellar structure under the Snyder-Oppenheimer scheme. Due to the homogeneity and isotropy of the model, we choose study the case of a closed geometry described by k=1, through the tool of dynamical systems. We revisit the different components of the star and its evolution during the stellar collapse, paying particular attention to the non-local effects and the quadratic terms of the energy momentum tensor that come from branes corrections. In the same vein we realize a phase portrait together with a stability analysis with the aim of obtain information about the attractors or saddle points of the dynamical system under different initial conditions in the density parameters, remarking the parameters that come from branes contributions.

Keywords: Brane theory; astrophysics

PACS: 04.50.-h; 04.40.Dg


Brane-world theory, is one of the most promising extensions to General Relativity (GR) due of their natural ability to solve fundamental problems in physics with unprecedented success1,2,3. One of the problems addressed in this context, is for example, the hierarchy problem which is solved by the insertion of one or two 4-dimensional branes in a 5-dimensional bulk with Anti d’Sitter (AdS) geometry (see for example) or a most complex bulk geometry 6; due to this particular topology, the gravity is weakened as it approaches to our 4-dimensional manifold (brane), solving in a natural way the problem of hierarchy 5,6. It is important to remark that this new topology generates modifications in Einstein’s equations with the presence of second order term in the energy-momentum tensor, the presence of bulk matter and the existence of nonlocal terms due to the 5-dimensional Weyl tensor 6.

From here, it is noteworthy to remark the contributions to cosmology7,8,9,10,11 and astrophysics12,13,14,15,16,17,18,19, establishing new dynamics and alternative solutions to for example, the stellar stability, dark energy and dark matter problems20,21,22,23,24,25,26. In cosmological context, it is possible to find quadratic terms and non local terms, which are relevant at high energies, providing new dynamic in inflationary models27 among others cosmological studies. Also we have new astrophysical dynamics from the brane-world point of view, where it is possible to explore the stability bounds generated by the presence of extra dimensions12,17,18, or the behavior of a star with a polytropic Equation of State (EoS)28.

There have been advances in this approach, where it is studied the stellar stability imposing different exterior conditions 12, there are also studies where it is considered a star with constant energy density in which is demonstrated that Schwarzschild exterior is the extreme case possible(see for example 17), also it is demonstrated the minimal setup to obtain a stellar configuration with the initial conditions of any EoS and with a Schwarzschild exterior17. As a counterpart, it is possible to study stellar collapse using the Snyder-Oppenheimer (SO) model through a no-go theorem in order to explore whether it is possible to maintain a Schwarzschild exterior type15. In the same vein, other studies focus in the gravitational collapse and black hole formation and evolution29 as well as the curvature corrections in the stellar collapse30.

Before we start, let us mention here some experimental constraints on braneworld models, most of them about the so-called brane tension, λ, which appears explicitly as a free parameter in the corrections of the gravitational equations mentioned above. As a first example we have the measurements on the deviations from Newton’s law of the gravitational interaction at small distances. It is reported that no deviation is observed for distances l0.1mm, which then implies a lower limit on the brane tension in the Randall-Sundrum II model (RSII): λ>1 TeV431; it is important to mention that these limits do not apply to the two-branes case of the Randall-Sundrum I model (RSI) (see 1 for details). Astrophysical studies, related to gravitational waves and stellar stability, constrain the brane tension to be λ>5×108 MeV412,32, whereas the existence of black hole X-ray binaries suggests that l10-2 mm 1,33. Finally, from cosmological observations, the requirement of successful nucleosynthesis provides the lower limit λ>1 MeV4, which is a much weaker limit as compared to other experiments (another cosmological tests can be seen in: Ref. 34).

Based in this background, this paper is dedicated to study the SO collapse in brane-world point of view through the theory of dynamical systems. We follow the standard procedure35 and it is extended to the case of branes with the aim of delve the behavior of the various components of the star at different stages of collapse, showing the critical points, stability and saddle points, remarking the advantage of this method to describe the dynamic of the star in its final stages36,37.

This paper is organized as follows: in Sec. 2 we show the mathematical formalism necessary for the study of brane theory. In Sec. 3 we explore the model of SO collapse in brane context, performance the results through a numerical analysis. Finally in Sec. 4 we discuss our results obtained throughout the paper. Henceforth we use units in which c==1.

2. Mathematical Background

Let us start by writing the equations of motion for stellar stability in a brane embedded in a 5D bulk according to the RSII model [6]. Following an appropriate computation (for details see 1,6), it is possible to demonstrate that the modified 4D Einstein’s equation can be written as

Gμν+Λ(4)gμν=κ(4)2Tμν+κ(5)4Πμν+κ(5)2Fμν-ξμν, 1

here Tμν is the four-dimensional energy-momentum tensor of the matter in the brane, Λ(4) is the four dimensional cosmological constant and κ(4) is the four dimensional coupling constant which is related with the five dimensional coupling constant κ(5), through the relation κ(4)2=8πGN=κ(5)4λ/6, where λ is the brane tension parameter and GN is the Newton constant. Also we have that Πμν represents the quadratic corrections on the brane generated from the four-dimensional energy-momentum tensor Tμν, whereas Fμν gives the contributions of the energy-momentum tensor in the bulk TAB (with latin letters taking values 0,1,2,3,4), which is then projected onto the brane with the help of the unit normal vector nA. Finally, ξμν gives the contributions of the five-dimensional Weyl’s tensor (5)CAFBE when projected onto the brane manifold (see 6 for more details).

For simplicity, we will not consider bulk matter and then TAB=0, which translates into Fμν=0, and will also discard the presence of the four-dimensional cosmological constant, Λ(4)=0, as we do not expect it to have any important effect at astrophysical scales (for a recent discussion about this see 38). The energy-momentum tensor Tμν, the quadratic energy-momentum tensor Πμν, and the Weyl (traceless) contribution ξμν, have the explicit forms:

Tμν=ρuμuν+phμν,Πμν=112ρ[ρuμuν+(ρ+2p)hμν],ξμν=-κ(5)κ(4)4[Uuμuν+Prμrν+hμν3(U+P)], 2

where p and ρ are, respectively, the pressure and energy density of the stellar matter of interest, U is the nonlocal energy density, P is the nonlocal anisotropic stress, u α the four-velocity (that also satisfies the condition gμνuμuν=-1), rμ is a unit radial vector and hμν=gμν+uμuν is the projection operator orthogonal to uμ. In this case we are assuming spherical symmetry for a real star.

3. Snyder-Oppenheimer collapse in branes

We turn our attention to the gravitational collapse of a ball made of dust, and look for the dynamic caused by the brane corrections15. Our arguments below will follow the simple assumptions we have made so far about the brane corrections on the 4-dimensional gravitational equations of motion. To begin with, we find it convenient to write the physical basis of a comoving coordinate system in the form:

ds2=-dt2+U(r,t)dr2+V(r,t)(dθ2+sin2(θ)dφ2). 3

For practical porpoises, it is possible rewrite Eq. in the form:

Rμν=κ(4)2(Tμν-12gμνT)+κ(5)4(Πμν-12gμνΠ)-ξμν, 4

then, the non-null terms are:

U˙V˙2UV-U˙24U2+U¨2U-1U[V''V-V'22V2-U'V'2UV]=4πGNρeff,V˙U˙4VU+V¨2V+1V-1U[V''2V-U'V'4UV]=4πGNρeff,U˙24U2+V˙22V2-U¨2U-V¨V=4πGNρeff,V'V˙2V2+U˙V'2UV-V˙'V=0, 5

where dots represents derivative with respect to t and primes represents derivatives with respect to r. We have also that ρeff and peff are defined as:

ρeff=ρ1+ρ2λ+Vλ, 6

peff=p1+ρλ+ρ22λ+V3λ+Nλ, 7

being V=U/κ(4)4 and N=4P/κ(4)4. In order to demonstrate the general conditions for stellar collapse, we start considering the following separable solution: U=R2(t)f(r) and V=S2(t)g(r); notice that requires: S(t)=R(t), where f and g can be normalized.

Under the argument that we are still free to redefine the radial coordinate as an arbitrary function of r (see [35] for details), it is possible to write: U=R2f(r), V=R2(t)r2. Using Eqs. and we have:

f'rf2=-1r2+1fr2-f'2rf2=-2k, 8

where prime denotes derivative with respect to r. Solving Eq. we have f(r)=(1-kr2)-1, obtaining a spatially homogeneous and isotropic metric

ds2=-dt2+R2(t)dr21-kr2+r2(dθ2+sin2(θ)dφ2), 9

here R(t) is the evolving scale factor of the star and k is associated with the geometry of the stellar configuration in equivalence with cosmology. The 4-dimensional Bianchi identities implies νTμνeff=0 and from the conservation equations we get νTμν=0, even more for a spatially homogeneous and isotropic Friedman model we have: νU=Pμν=0 (see39 for details). Then, it is possible to extract information about ρ(t) and V(t) through the following conservation equations:

ρ̇+3Hρ=0,V̇+4HV=0, 10

here the dot represents derivative with respect to t and we define HṘ/R. From Eqs. we obtain ρ(t)=ρ0R(t)-3 and V(t)=V0R(t)-4. Substituting in and solving for Ṙ we have

H2=-k+κ(4)23ρ0R31+ρ02λR3+V0λR4. 11

Notice that in the GR regime ( ρ0/λ0, V0/λ0) with k0, we recover the parametric solution of cycloid reported in the literature35. In general, Eq. can be solved by quadratures giving the following expression:

t-t0=2(-1)1/6α1/39(3)1/4α+x3(-1)5/6(-1)1/3xα1/3-11/2(-1)2/3x2α2/3+(-1)1/3xα1/3+11/2×Farcsin(3)-1/4-(-1)5/6xα1/3-(-1)5/6,(-1)1/3, 12

where α-ax6+bx2+c, being a3/κ(4)2ρ0, bV0/ρ0λ, cρ0/2λ, x(3/κ(4)2ρ0)1/2R3 and F(z,y) is the Elliptic function, under the assumption of a closed geometry k=1, in concordance with conventional wisdom.

3.1. Dynamical Analysis

To complement this study, we analyze the equation of motion from the metric element(9), where the stellar components evolve during the collapse:

H(t)2=ρeff(t)-kρk(t), 13

where k(t)=1/R(t)2. In addition, we propose the following dimensionless variables

Ωmρ¯H2,ΩVVH2λ,Ωλρ2λ,ΩkρkH2, 14

subject to the Friedman condition

1+kΩk=Ωm(1+Ωλ)+ΩV. 15

The dynamical system can be written as:

Ωm'Ωm=-3-2Π,ΩV'ΩV=-4-2Π,Ωλ'Ωλ=-3,Ωk'Ωk=-2-2Π, 16

where now, the primes denote derivative with respect to the e-foldings ( N=ln(R)) and Π is defined as

ΠH'H=-32Ωm(1+2Ωλ)-2ΩV+kΩk, 17

which can be obtained from Eq.(13) . From conditions (14) and (15), it is enough to investigate the flow of (16) defined in the space phase

Ψ={(Ωm,Ωλ,Ωk):0Ωm(1+Ωλ)-kΩk1,0Ωm1,0Ωλ1,0Ωk1}, 18

where it is reduced the above condition due that we assume 0ΩV1.

Before to start, we establish two important limits: The first one, is the low energy limit where GR is recovered; in this case we have that Ωλ1 and ΩV0 recovering the SO collapse obtained form classical GR. In the other case, brane effects begin to be significant, dominating over the other terms. Then, Eq. and the Friedman constraint can be expressed as: 1+kΩk=ΩmΩλ+ΩV together with

ΠHigh=-3ΩmΩλ-2ΩV+kΩk. 19

Returning to our analysis, Eqs.(16a)-(17) are readily soluble analytically, under the assumption k=0 due to the spherical geometry of the stellar configuration. The results are shown in Fig. 1. In the first case (Fig. 1 Top) we have that the initial conditions imposed are: Ωm0=0.8, ΩV0=0.15, Ωλ0=0.3 and Ωk0=0.25, where it is possible to observe the domination of baryonic matter. In the second case (Fig. 1 Bottom) brane parameters are dominant over the other components, having the initial conditions: Ωm0=0.1, ΩV0=0.5, Ωλ0=0.4 and Ωk0=0.25. It is possible to observe that the non-local term is always dominant until the final stages of the stellar collapse. Both initial conditions are chosen by hand, only by the premise of show the behavior of the components under different conditions.

Figure 1 Phase space of the system (16a)-(16b), for the spherical geometry k = 1. (Top) Here we assume dominance of baryonic density parameter in comparison with the other components, as expected in a real stellar configuration. It is shown the matter, Weyl, brane tension and curvature terms during the evolution of collapse of the star. Notice how the high energy term Ωλ always dominate in the closest moments of collapse. (Bottom) In this case we assume that brane corrections are dominant over the other components, maintaining the presence of non local terms until the final stages of collapse; the brane tension parameter always grow exponentially as we expect. 

It is important to notice, how Fig. 1 show that the brane term Ωλ grow exponentially in comparison with the other components; this behavior is due that the direct integration, image generates an exponential function described in the following way: Ωλ=Ωλ0exp(-3N), notice how the other components are negligible nearest to the collapse.

To complement our study realized through this section, we analyze the equilibrium points and eigenvalues associated to Eqs.(16) and (16b) in order to obtain important information about the collapse behavior. It is possible to define the equation of critical points as: (dΩi/dN)x0=0. In this case we have three critical points with matter, Weyl fluid and curvature domination, shown in Table I. Also, we define the vector x=(Ωm,ΩV,Ωλ,Ωk) and consider a linear perturbation of the form xxc+δx. The linearized system reduces to δ x'=Jδx, where J is the Jacobian matrix of x', written as:

J=Ωi'Ωjx0=-3-2[Π0-32Ωm0(1+2Ωλ0)]4Ωm06Ωm02-2kΩm03ΩV0(1+2Ωλ0)-4-2(Π0-2ΩV0)6ΩV0Ωm0-2kΩV000-303Ωk0(1+2Ωλ0)4Ωk06Ωk0Ωm0-2-2(Π0+kΩk0) 20

Table I Critical points for the system (16a) and (16b). From left to right, the columns read: Point, coordinates, existence, eigenvalues and stability. 

In order to obtain information about attractors, saddle points and others, we found the eigenvalues associated with the Jacobian matrix . Table I summarize the eigenvalues associated with this particular model and establish the conditions of the eigenvalues existence (see the middle part of Table I). Our results remark the existence of saddle-like points in dynamics which represents unstable manifolds, being notorious in Figs. 2 which are phase portrait of Eqs.(16a)-(16b).

Figure 2 Phase portrait of Eqs. (16a)-(16b). (Top) As initial conditions, we fix the value of the matter density parameter at Ωm= 0.7 and the other two density parameters vary in the interval Ωkϵ[0:2; 0:4] and Ωλϵ[0:2; 0:4] always maintaining the dominance of the matter density parameter. (Bottom) In this case we fix Ωk=0.25 and varying the other two parameters in the intervals Ωmϵ[0:25; 0:8] and Ωλϵ[0:15; 0:7], from here it is possible to see two saddle points unlike the previous case. 

Figures were computed under the following Initial conditions: In Fig. 2 top we fix the value of the matter density parameter at Ωm0=0.7 and the other two density parameters vary in the interval ΩV0ϵ[0.2,0.4] and Ωk0ϵ[0.2,0.4] always maintaining the dominance of the matter density parameter. In the same vein, for Fig. 2 bottom, we analyze the behavior, fixing Ωk0=0.25 and varying the other two parameters in the intervals Ωm0ϵ[0.25,0.8] and ΩV0ϵ[0.15,0.7]. In both cases we fix the brane tension density parameter as: Ωλ0=0.3. Finally in Fig. 3 we apply the initial conditions ΩV0=0 with Ωm0ϵ[0.25,0.8] and Ωk0ϵ[0.25,0.8], such that the only term in which it contributes branes is Ωλ0=0.3.

Figure 3 Phase portrait of Eqs. (16a)-(16b). we apply the initial conditions Ωvo=0 with Ωm0ϵ[0:25; 0:8] and Ωkoϵ[0:25; 0:8], such that the only term in which it contributes branes is Ωλo=3

4. Discussion

In this paper we implement a roboust analysis of the SO collapse in the background of branes showing the new terms that will play a role in the dynamic of collapse of a star. We start with the equation of motion for SO collapse which is shown in Eq. (11) and solved analytically for the most general case where branes play an important role, never losing sigh that Eq. (11) and Eq. (11) converge to GR in the appropriate limit ρ0/λ0 and V0/λ0.

Similar analysis was conducted from the point of view of dynamical systems in order to study the dynamics of the different components of the star. In this case, we focused on the matter components (dust), the brane terms thats grows proportional to ρ/λ, the non-local terms due to the Weyl tensor and the geometrical term fixed only in the spherical geometry k=1. From this study, it was possible to extract relevant information regarding the behavior of stellar collapse with the addition of terms that come from brane-worlds. In this case, we impose reasonable conditions that must contain a star in the most natural possible conditions. As it was expected, the brane term associated with Ωλ must dominate over the other density parameters due to its exponential behavior, allowing the natural decaying of the other components in the final stages of the stellar collapse. Notoriously, Weyl terms only dominates slightly in the final stage but always is subdominant previous the collapse as we expect from the traditional knowledge of stellar dynamics. On the other hand, we explore the dynamic when the brane components are dominant over the other components, showing the dominance of the Weyl term even in the final stages of the collapse.

To complement, we realize the phase portrait of Eqs.(16a)-(16b) (see Figs. 2 and 3) assuming different initial conditions with the aim of prove the behavior under different conditions. The mathematical and numerical analysis show saddle points which are unstable in the dynamics, noticing that the presence of non-local terms generates the discontinuity presented in Figs. 2. From Fig. 3 the plot is only restricted to the plane Ωk, Ωm due to the condition ΩV0=0; despite this, the presence of branes still there, mediated by the term Ωλ.

As a final note, we emphasize that the procedure can be replicated for other classes of stars that may include the presence of polytropic matter or with other most general focuses and whose solutions may also require extra numerical analysis. However this is ongoing research that will be presented elsewhere.


The authors acknowledge support from SNI-México, PIFI and PROMEP with number CA 205. MAG-A acknowledge support from CONACyT research fellow, Instituto Avanzado de Cosmología (IAC) collaborations. JCL-D acknowledge support from F-PROMEP-39/Rev-03. MJR-Iacknowledges support from a CONACyT postdoctoral grant.


1. R. Maartens and K. Koyama, Living Rev. Rel. 13 (2010) 5. arXiv: 1004.3962 [hep-th]. [ Links ]

2. A. Perez-Lorenzana, (2004) arXiv: hep-ph/0406279 [hepph]. [ Links ]

3. A. Mazumdar, Phys. Rev. D64 (2001) 027304, arXiv: hep-ph/0007269 [hep-ph]. [ Links ]

4. M. Gogberashvili, Int. J. Mod. Phys. D11 (2002) 1635. arXiv: hep-ph/9812296 [hep-ph]. [ Links ]

5. L. Randall and R. Sundrum, Phys. Rev. Lett. 3370 (1999) 83. arXiv: hep-ph/9905221. [ Links ]

6. L. Randall and R. Sundrum, Phys. Rev. Lett. 83 (1999) 4690. arXiv: hep-th/9906064 [hep-th]; T. Shiromizu, K.-i. Maeda, and M. Sasaki, Phys. Rev. D62 024012 (2000), arXiv: gr-qc/9910076 [gr-qc]. [ Links ]

7. P. Binetruy, C. Deffayet, U. Ellwanger, and D. Langlois, Phys. Lett. B477 (2000) 285. arXiv: hep-th/9910219 [hep-th]. [ Links ]

8. A. Wang, R.-G. Cai, and N. Santos, (2006). arXiv: astroph/0607371 [astro-ph]. [ Links ]

9. P. Binetruy, C. Deffayet, and D. Langlois, Nucl. Phys. B565 (2000) 269. arXiv: hep-th/9905012 [hep-th]. [ Links ]

10. M.A. García-Aspeitia and T. Matos, Gen. Rel. Grav. 43 (2011) 315. arXiv: 0906.3278 [gr-qc]. [ Links ]

11. M.A. Garcia-Aspeitia, J. Magana, and T. Matos, Gen. Rel. Grav. 44 (2012) 581. arXiv: 1102.0825 [gr-qc]. [ Links ]

12. C. Germani and R. Maartens, Phys. Rev. D64 (2001) 124010. arXiv: hep-th/0107011 [hep-th]. [ Links ]

13. M.A. Garcia-Aspeitia, Rev. Mex. Fis. 60 (2014) 205. arXiv: 13 06.1283 [gr-qc]. [ Links ]

14. F. Linares, Master Thesis (2013). [ Links ]

15. M. Bruni, C. Germani, and R. Maartens, Phys. Rev. Lett. 87 (2001) 231302. arXiv: gr-qc/0108013 [gr-qc]. [ Links ]

16. L. Gergely, T. Harko, M. Dwornik, G. Kupi, and Z. Keresztes, Mon. Not. Roy. Astron. Soc. 415 (2011) 3275., arXiv: 1105.0159 [gr-qc] . [ Links ]

17. M.A. García-Aspeitia and L.A. Urena López, Class. Quantum Grav. 32 (2014) 025014. arXiv: 1405.3932 [grqc]. [ Links ]

18. F.X. Linares, M.A. García-Aspeitia, and L. A. Urena López, Phys. Rev. D92 (2015) 024037. [ Links ]

19. J. Ovalle, L. Gergely, and R. Casadio, (2014). arXiv: 1405.0252 [gr-qc]. [ Links ]

20. A. Lue and G. Starkman, Phys. Rev. D67 (2003) 064002. arXiv: astro-ph/0212083 [astro-ph]. [ Links ]

21. J.A.R. Cembranos, A. Dobado, and A.L. Maroto, Phys. Rev. Lett. 90 (2003) 241301. [ Links ]

22. N. Okada and O. Seto, Phys. Rev. D70 (2004) 083531. arXiv: hep-ph/0407092 [hep-ph]. [ Links ]

23. J.-M. Schwindt and C. Wetterich, Nucl. Phys. B726 (2005) 75. arXiv: hep-th/0501049 [hep-th]. [ Links ]

24. S. Chakraborty, A. Banerjee, and T. Bandyopadhyay, (2007). arXiv: 0707.0199 [gr-qc]. [ Links ]

25. M. Sano and H. Suzuki, Phys. Rev. D81 (2010) 024042. arXiv: 0907.2495 [hep-th]. [ Links ]

26. S. Shahidi and H.R. Sepangi, Int. J. Mod. Phys. D20 (2011) 77. arXiv: 1009.5458 [gr-qc]. [ Links ]

27. R. Maartens, V. Sahni, and T. D. Saini, Phys. Rev. D63 (2001) 063509, arXiv: gr-qc/0011105 [gr-qc]; R. Maartens, D. Wands, B. A. Bassett, and I. Heard, ibid. D62 (2000) 041301, arXiv: hep-ph/9912464 [hepph]; T. Gonzalez, T. Matos, I. Quiros, and A. Vazquez- Gonzalez, Phys. Lett. B676 (2009) 161. arXiv: 0812.1734 [gr-qc]. [ Links ]

28. L.B. Castro, M.D. Alloy, and D.P. Menezes, JCAP 1408 (2014) 047. arXiv:1403.1099 [nucl-th]. [ Links ]

29. R. Casadio and C. Germani, Prog. Theor. Phys. 114 (2005) 23. arXiv: hep-th/0407191 [hep-th]. [ Links ]

30. G. Kofinas and E. Papantonopoulos, JCAP 0412 (2004) 011. arXiv: gr-qc/0401047 [gr-qc]. [ Links ]

31. D. Kapner et al., Phys. Rev. Lett. 98 (2007) 021101, arXiv: hep-ph/0611184 [hep-ph]; S. Alexeyev, K. Rannu, P. Dyadina, B. Latosh, and S. Turyshev, (2015), 10.7868/S00444510150600 51, arXiv: 1501.04217 [gr-qc]. [ Links ]

32. J. Sakstein, B. Jain, and V. Vikram, Int. J. Mod. Phys. D 23 (2014) 1442002. arXiv: 1409.3708 [astro-ph.CO]. [ Links ]

33. H. Kudoh, T. Tanaka, and T. Nakamura, Phys. Rev. D68 (2003) 024035. arXiv: gr-qc/0301089 [gr-qc]; M. Cavaglia, Int. J. Mod. Phys. A18 (2003) 1843. arXiv: hep-ph/0210296 [hep-ph]. [ Links ]

34. R. Holanda, J. Silva, and F. Dahia, Class. Quant. Grav. 30 (2013) 205003. arXiv: 1304.4746 [astro-ph.CO]; J. D. Barrow and R. Maartens, Phys. Lett. B532 (2002) 153. arXiv: gr-qc/0108073 [gr-qc]; P. Brax and C. van de Bruck, Class. Quant. Grav. 20 (2003) R201. arXiv: hepth/ 0303095 [hep-th]. [ Links ]

35. S. Weinberg, Gravitation and Cosmology (John Wiley & Sons, 1972). [ Links ]

36. D. Escobar, C.R. Fadragas, G. Leon, and Y. Leyva, Class. Quant. Grav. 29 (2012) 175005. arXiv: 1110.1736 [gr-qc]. [ Links ]

37. D. Escobar, C. R. Fadragas, G. Leon, and Y. Leyva, Class. Quant. Grav. 29 (2012) 175006. arXiv: 1201.5672 [gr-qc]. [ Links ]

38. V. Pavlidou and T.N. Tomaras, (2013). arXiv: 1310.1920 [astro-ph.CO]. [ Links ]

39. R. Maartens, Phys. Rev. D62 (2000) 084023. arXiv: hepth/000 4166 [hep-th]. [ Links ]

Received: July 29, 2015; Accepted: January 04, 2016

Creative Commons License This is an open-access article distributed under the terms of the Creative Commons Attribution License