Advances in High Energy Physics

Volume 2019, Article ID 5234014, 11 pages

https://doi.org/10.1155/2019/5234014

## Dark Energy in Spherically Symmetric Universe Coupled with Brans-Dicke Scalar Field

^{1}Department of Mathematics, Mizoram University, Aizawl, Mizoram 796004, India^{2}Department of Mathematics, BITS Pilani K K Birla Goa Campus, Goa 403726, India

Correspondence should be addressed to Gauranga C. Samanta; moc.liamg@18agnaruag

Received 5 March 2019; Accepted 27 March 2019; Published 2 May 2019

Guest Editor: Subhajit Saha

Copyright © 2019 Koijam Manihar Singh and Gauranga C. Samanta. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.

#### Abstract

The phenomenon of dark energy and its manifestations are studied in a spherically symmetric universe considering the Brans-Dicke scalar tensor theory. In the first model, the dark energy behaves like a phantom type and in such a universe the existence of negative time is validated with an indication that our universe started its evolution before . Dark energy prevalent in this universe is found to be more active at times when other types of energies remain passive. The second model of universe begins with big bang. On the other hand, the dark energy prevalent in the third model is found to be of the quintessence type. Here, it is seen that the dark energy triggers the big bang and after that much of the dark energy reduces to dark matter. One peculiarity in such a model is that the scalar field is prevalent eternally; it never tends to zero.

#### 1. Introduction

The type Ia (SNIa) supernovae observations suggested that our universe is not only expanding, but also the rate of expansion is in accelerating way [1, 2] and this acceleration is caused by some mysterious object, so called dark energy. The matter species in the universe are broadly classified into relativistic particle, nonrelativistic particle, and dark energy. Another component, apparently a scalar field, dominated during the period of inflation in the early universe. In the present universe, the sum of the density parameters of baryons, radiation, and dark matter does not exceed 30% [3]; we still need to identify the remaining 70% of the cosmic matter. We call this 70% unknown component as dark energy, and it is supposed to be responsible for the present cosmic acceleration of the universe. According to the cosmological principle, our universe is homogeneous and isotropic in large scale. By assuming isotropicity and homogeneity, the acceleration equation of the universe in general theory of relativity can be written as . The acceleration and deceleration of the universe depend on the sign of ; that is, the universe will accelerate if or decelerate if . So, the condition has to be satisfied in general relativity to explain accelerated expansion of the universe. This implies that the strong energy condition is violated; moreover, the strong energy condition is violated, meaning that the universe contains some abnormal (something not normal) matter. Hence, without violating strong energy condition, the accelerated expansion of the universe is not possible in general theory of relativity. Therefore, the modification of the general theory of relativity is necessary. Essentially, there are two approaches, out of which one is to modify the right-hand side of Einstein’s field equations (i.e., matter part of the universe) by considering some specific forms of the energy momentum tensor having a huge negative pressure and which is concluded in the form of some mysterious energy dubbed as dark energy. In this approach, the simplest candidate for dark energy is cosmological constant , which is described by the equation of state [4]. The second approach is by modifying Einstein Hilbert action, that is, the geometry of the space-time, which is named as modified gravity theory. So many modifications of general relativity theory have been done, namely, Brans-Dicke (BD) [5] and Saez-Ballester scalar-tensor theories [6], gravity [7–12], gravity [13–16], Gauss-Bonnet theory [17–20], Horava-Lifshitz gravity [21–23], and recently gravity [24]. Subsequently, so many authors [25–54] have been studying modified gravity theory to understand the nature of the dark energy and accelerated expansion of the universe.

Apart from this, the Hubble parameter may provide some important information about the evolution of our universe. It is dynamically determined by the Friedmann equations and then evolves with cosmological red-shift. The evolution of Hubble parameter is closely related with radiation, baryon, cold dark matter, and dark energy or even other exotic components available in the universe. Further, it may be impacted by some interactions between these cosmic inventories. Thus, one can look out upon the evolution of the universe by studying the Hubble parameter. Besides dark energy, there exists a dark matter component of the universe. One can verify whether these two components can interact with each other. Theoretically, there is no evidence against their interaction. Basically, they may exchange their energy which affects the cosmic evolution of the universe. Furthermore, it is not clear whether the nongravitational interactions between two energy sources produced by two different matters in our universe can produce acceleration. We can assume for a while that the origin of nongravitational interaction is related to emergence of the space-time dynamics. However, this is not of much help, since this hypothesis is not more fundamental compared with other phenomenological assumptions within modern cosmology [55–59]. However, the authors [60, 61] studied the finding that the interacting cosmological models make good agreement with observational data. The aim of this paper is to study a cosmological model, where a phenomenological form of nongravitational interactions is involved. In this article, we are interested in the problem of accelerated expansion of the large-scale universe; we follow the well-known approximation of the energy content of the recent universe. Namely, we consider the interaction between dark energy and other matters (including dark matter).

#### 2. Space-Time and Field Equations

We consider the spherically symmetric space-timewhere is a function of time. The energy momentum tensor for the fluid comprising our universe is taken aswhere and are, respectively, the total energy density and total pressure which are taken asandwith and being, respectively, the densities of dark energy and other matters in this universe. and are, respectively, the pressures of dark energy and other matters (including dark matter) in this universe. And is the flow vector satisfying the relationsThe Brans-Dicke scalar tensor field equations are given bywithwhere is the coupling constant and is the scalar field. Energy conservation gives the equationHere the field equations take the formHere, we take the equation of state parameter for dark energy as so thatAnd the conservation equation givesSince the dark energy and other matters are interacting in this universe, (14) can be written asandwhere is the interaction between dark energy and other matters (including dark matter) which this universe comprises. Here can take different forms like , , , and so forth, where is a coupling constant. It can also take other forms which are functions of and . Now from (10) and (11) we get the relationwhich giveswhere is an arbitrary constant.

#### 3. Analytical Solutions

In this section, we try to obtain the analytical solutions of the field equations in three different cases based on the different forms of the interaction parameter .

##### 3.1. Case-I

From (17) and (18) we getwhere , , , and are arbitrary constants. Here in this case we takewhere is Hubble’s parameter so that the conservation equation takes the form of the equationsandNow from (23) we getwhere is an arbitrary constant andThus using (24) in (9) we haveTherefore (22) givesNow using (27) in (10) we haveAgain from (13) and (24) we getThus comparing coefficients of and of the two expressions of in (28) and (29), we obtainwhich is automatically satisfied; andIn this caseAnd the interaction is given byThe physical and kinematical properties of the model are obtained as follows:

Volume is

Hubble’s parameter is

Expansion factor is

Deceleration parameter is

Jerk parameter is

And state-finder parameters are obtained as

Dark energy parameter is

##### 3.2. Case-II

As another solution we get from (17) and (18),where , , and are arbitrary constants. Here in the case we take the interaction aswhere is the mean Hubble’s parameter. Then (15) and (16), respectively, take the formsandFrom (46) we getwhere is an arbitrary constant. Now using (42), (43), and (47) in (9) we getHere, using (47), (48) and (13), (12) gives In this caseAnd the interaction is obtained as

##### 3.3. Case-II(a)

In this case, we take the interaction as , so that the conservation equations take the formsNow, from (9), using (42) and (43), we get From (53), using (54), (13) and (42), we have whereAnd this is possible without loss of generality as can take values such that as well as which is the characteristic of different forms of dark energy which can be attained according to different values of . Now (55) givesFrom (54) and (57), we haveNow from (57) and (13) we takeThus, now using (59) in (10), we getAnd in this caseHere the interaction is obtained asThe physical and kinematical properties of the models are as follows:

##### 3.4. Case-III

Equations (17) and (18) giveHere in this case we assume the interaction between dark energy and other matters of the universe in the formso that (15) and (16), respectively, take the formsNow from (9) we getThus, from (74) and (75), using relation (13), we havewhereAgain using relations (70), (71), (75), (76), and (13) in (12), we haveHereAndIn this case, the interaction is given byThe physical and kinematical properties of the model are obtained as follows:

#### 4. Study of the Solutions and Conclusions

For the model universe in Case-I, we see that, at , the energy density has finite value dependent on the coupling constant of the interaction between dark energy and other matters in this universe, and the total energy density is found to decrease with time until it tends to zero at infinite time and the interaction term is also found to follow the same behavior with respect to time. But during this time the rate of decrease of the dark energy density is slower in comparison to the rate of decrease of the energy density of other matters in the universe. Therefore, as time passes by, dark energy seems to dominate over other matters. Thus, the scenario in such type of universe is that dark energy plays a vital role and it seems that as the energy density of dark energy increases the expansion of the universe increases.

In this model, it is seen that, at , , which shows that if we have to accept the big bang theory, the universe begins its evolution at time , thereby implying the existence of negative time which is almost possible from the presence of dark energy in this universe. Again the value of the deceleration parameter obtained here implies that the value of is limited by the condition . And in this model the expansion of the universe is accelerating though the rate decreases with time. Therefore, this universe may be taken as a reasonable model; otherwise, if the rate of expansion increases with time, there will be a singularity where the universe ends transforming itself into a cloud of dust.

In this universe, we see that the interaction between dark energy and other matters decreases with time, and perhaps there is a tendency where the dark energy decays into cold dark matter. Again it is seen that dark energy density is zero only at time showing that dark energy exists before also. Thus perhaps there exists an epoch before our cosmic time begins in the history of evolution of the universe.

Here, in this case, if either or , then we get the state-finder parameter as and for which the dark energy model reduces to a flat model which predicts a highly accelerated expansion before these events of time. In this model, the interaction between dark energy and other matters is found to exist at these events of time not interrupted by the high speed of expansion.

For this universe, the equation of state parameter for dark energy is found to be less than which indicates that the dark energy contained is of the phantom type. From the study of the interaction, we also see that the action of such type of dark energy is more when the energies from other types of sources remain idle or not so active. It is also opposite to or against the light energy. It acts also against the living energy or the energy possessed by the human beings.

In Case-II, though the universe is expanding and the rate of expansion is accelerating, it depends much on the value of , which indicates that the expansion is related to the dark energy density. There it may be taken that dark energy enhances the accelerated expansion. And this enhancement is also dependent on the value of which is the coupling constant of the interaction between dark energy and other matters in this universe. This implies that the expansion of the universe is very much interrelated with the interaction between dark energy and other components of the universe. Thus, all the members of this universe may be taken to expand due to also the presence of dark energy. Hence, considering a small-scale structure of the universe, the earth may be taken to expand due to also the presence of dark energy.

In this universe, we see that when , it goes to the asymptotic static era with and . And when , the universe goes to model for which and . Thus, the state-finder parameters show the picture of the evolution of our universe, starting from the asymptotic static era and then coming to the model era. Here we see that the interaction as which means that the interaction almost stops at the cosmic time when the scale factor of the universe becomes or takes the value .

Again it is seen that the energy density of this model universe tends to infinity at and decreases gradually as ; thus it seems that our universe started with a big bang. From the above behaviors of this model, it is also implied that at the beginning of the evolution of this universe there was no interaction between dark energy and other components of the universe, and after that the interaction between them becomes active and increases with time, and at present they are highly interacting. But this interaction also depends much on the values of and which are, respectively, equation of state parameter of the dark energy contained and the coupling constant of interaction.

Case-III represents the logamediate scenario of the universe where the cosmological solutions have indefinite expansion [62]. In this case, the dark energy has a quintessence-like behavior. Here the matter content of the universe is seen to increase slowly due to the interaction and the cosmic effect. In this universe, there is an interesting event of time, that is, the cosmic time, when . At this point, the universe has the tendency of accelerating expansion, but the expansion suddenly stops at this moment and the volume of the universe takes the value of 1 at this juncture. So it seems that there is a bounce and a new epoch begins from this juncture. Also we see that, at , the state-finder parameters take the values and . Thus at this instant our universe will go to that of a model which implies that at this event of time most of the dark energy contained will reduce to cold dark matter.

The energy density of this model universe tends to infinity at which indicates that this universe begins with a big bang, and it (energy density) decreases gradually until it tends to a finite quantity at infinite time, of course with a bounce at . And at , the dark energy density is found to be exceptionally high which indicates that it helps much in triggering the big bang. It is also seen that the dark energy is highly interacting with other components of the universe at , with the interaction decreasing slowly with the passing away of the cosmic time. In this universe, we see that both the scalar field and the interaction tend to vanish as . Thus, the scalar field is very much interconnected with the dark energy content of this universe and plays a vital role in the production and existence of it. One peculiarity in this model is that the scalar field does not vanish at ; thus, the dark energy seems to be prevalent eternally in this universe due to this scalar field.

#### Data Availability

No data were used to support this study.

#### Conflicts of Interest

The authors declare that they have no conflicts of interest.

#### References

- A. G. Riess, A. V. Filippenko, P. Challis et al., “Observational evidence from supernovae for an accelerating universe and a cosmological constant,”
*The Astronomical Journal*, vol. 116, no. 3, pp. 1009–1038, 1998. View at Publisher · View at Google Scholar - S. Perlmutter, G. Aldering, G. Goldhaber et al., “Measurements of Ω and Λ from 42 high-redshift supernovae,”
*The Astrophysical Journal*, vol. 517, pp. 565–586, 1999. View at Publisher · View at Google Scholar - L. Amendola and S. Tsujikawa,
*Dark Energy: Theory and Observations*, Cambridge University Press, Cambridge, UK, 2010. View at Publisher · View at Google Scholar - S. Weinberg, “The cosmological constant problem,”
*Reviews of Modern Physics*, vol. 61, no. 1, pp. 1–23, 1989. View at Publisher · View at Google Scholar · View at MathSciNet - C. Brans and R. H. Dicke, “Mach's principle and a relativistic theory of gravitation,”
*Physical Review*, vol. 124, no. 3, pp. 925–935, 1961. View at Publisher · View at Google Scholar - D. Saez and V. J. Ballester, “A simple coupling with cosmological implications,”
*Physics Letters A*, vol. 113, no. 9, pp. 467–470, 1986. View at Publisher · View at Google Scholar - D. E. Barraco and V. H. Hamity, “Spherically symmetric solutions in theories of gravity obtained using the first order formalism,”
*Physical Review D*, vol. 62, no. 4, Article ID 044027, 6 pages, 2000. View at Publisher · View at Google Scholar - S. Capozziello, “Curvature quintessence,”
*International Journal of Modern Physics D*, vol. 11, pp. 483–492, 2002. View at Google Scholar - S. Capozziello, V. F. Cardone, and A. Troisi, “Reconciling dark energy models with
*f(R)*theories,”*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 71, no. 4, Article ID 043503, 2005. View at Publisher · View at Google Scholar - S. Capozziello, V. F. Cardone, and M. Francaviglia, “ theories of gravity in the Palatini approach matched with observations,”
*General Relativity and Gravitation*, vol. 38, no. 5, pp. 711–734, 2006. View at Publisher · View at Google Scholar · View at MathSciNet - S. Nojiri and S. D. Odintsov, “Modified gravity consistent with realistic cosmology: From a matter dominated epoch to a dark energy universe,”
*Physical Review D*, vol. 74, no. 8, Article ID 046004, 13 pages, 2006. View at Publisher · View at Google Scholar · View at Scopus - K. Bamba and C.-Q. Geng, “Thermodynamics in
*F(R)*gravity with phantom crossing,”*Physics Letters B: Particle Physics, Nuclear Physics and Cosmology*, vol. 679, no. 3, pp. 282–287, 2009. View at Google Scholar · View at MathSciNet - R. Ferraro and F. Fiorini, “Modified teleparallel gravity: inflation without an inflaton,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 75, no. 8, Article ID 084031, 2007. View at Publisher · View at Google Scholar · View at MathSciNet - R. Myrzakulov, “Accelerating universe from
*F(T)*gravity,”*The European Physical Journal C*, vol. 71, article 1752, 2011. View at Publisher · View at Google Scholar - K. Bamba, C.-Q. Geng, C.-C. Lee, and L.-W. Luo, “Equation of state for dark energy in
*f(T)*gravity,”*Journal of Cosmology and Astroparticle Physics*, vol. 2011, p. 21, 2011. View at Publisher · View at Google Scholar - M. R. Setare and F. Darabi, “Power-law solutions in
*f*(T) gravity,”*General Relativity and Gravitation*, vol. 44, no. 10, pp. 2521–2527, 2012. View at Publisher · View at Google Scholar · View at Scopus - S. Nojiri, S. D. Odintsov, and M. Sasaki, “Gauss-Bonnet dark energy,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 71, no. 12, Article ID 123509, 2005. View at Publisher · View at Google Scholar - L. M. Sokołowski, Z. A. Golda, M. Litterio, and L. Amendola, “Classical instability of the einstein-gauss-bonnet gravity theory with compactified higher dimensions,”
*International Journal of Modern Physics A*, vol. 6, no. 25, pp. 4517–4555, 1991. View at Publisher · View at Google Scholar - A. Iglesias and Z. Kakushadze, “Solitonic brane world with completely localized (super)gravity,”
*International Journal of Modern Physics A*, vol. 16, no. 21, pp. 3603–3631, 2001. View at Publisher · View at Google Scholar · View at MathSciNet - S. Nojiri, S. D. Odintsov, and S. Ogushi, “Friedmann-Robertson-Walker brane cosmological equations from the five-dimensional bulk (A)dS black hole,”
*International Journal of Modern Physics A*, vol. 17, no. 32, pp. 4809–4870, 2002. View at Publisher · View at Google Scholar · View at MathSciNet - E. Ó. Colgáin and H. Yavartanoo, “Dyonic solution of Hořava-Lifshitz gravity,”
*Journal of High Energy Physics*, vol. 2009, no. 08, p. 021, 2009. View at Publisher · View at Google Scholar - A. Ghodsi, “Toroidal solutions in hořava gravity,”
*International Journal of Modern Physics A*, vol. 26, no. 5, pp. 925–934, 2011. View at Publisher · View at Google Scholar - M. I. Park, “A test of Hořava gravity: the dark energy,”
*Journal of Cosmology and Astroparticle Physics*, vol. 2010, no. 01, p. 1, 2010. View at Publisher · View at Google Scholar - T. Harko, F. S. N. Lobo, S. Nojiri, and S. D. Odintsov, “
*F*(*R, T*) gravity,”*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 84, no. 2, Article ID 024020, 11 pages, 2011. View at Publisher · View at Google Scholar · View at Scopus - M. H. Dehghani, “Accelerated expansion of the Universe in Gauss-Bonnet gravity,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 70, no. 6, Article ID 064009, 6 pages, 2004. View at Publisher · View at Google Scholar · View at MathSciNet - S. Nojiri and S. D. Odintsov, “Modified gravity with ln
*R*terms and cosmic acceleration,”*General Relativity and Gravitation*, vol. 36, no. 8, pp. 1765–1780, 2004. View at Publisher · View at Google Scholar - A. Lue, R. Scoccimarro, and G. Starkman, “Probing Newton's constant on vast scales: Dvali-Gabadadze-Porrati gravity, cosmic acceleration, and large scale structure,”
*Physical Review D: Covering Particles, Fields, Gravitation, and Cosmology*, vol. 69, no. 12, Article ID 044005, 10 pages, 2004. View at Publisher · View at Google Scholar - S. M. Carroll, A. De Felice, V. Duvvuri, D. A. Easson, M. Trodden, and M. S. Turner, “Cosmology of generalized modified gravity models,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 71, no. 6, Article ID 063513, 2005. View at Publisher · View at Google Scholar - G. C. Samanta and S. N. Dhal, “Higher dimensional cosmological models filled with perfect fluid in
*f(R,T)*theory of gravity,”*International Journal of Theoretical Physics*, vol. 52, no. 4, p. 1334, 2013. View at Publisher · View at Google Scholar - G. C. Samanta, “Kantowski-sachs universe filled with perfect fluid in
*f(R,T)*theory of gravity,”*International Journal of Theoretical Physics*, vol. 52, no. 8, pp. 2647–2656, 2013. View at Publisher · View at Google Scholar - G. C. Samanta, “Universe filled with dark energy (DE) from a wet dark fluid (WDF) in
*f(R,T)*gravity,”*International Journal of Theoretical Physics*, vol. 52, no. 7, pp. 2303–2315, 2013. View at Publisher · View at Google Scholar - G. C. Samanta, “Holographic dark energy (DE) cosmological models with quintessence in bianchi type-V space time,”
*International Journal of Theoretical Physics*, vol. 52, no. 12, pp. 4389–4402, 2013. View at Publisher · View at Google Scholar - K. M. Singh and K. Priyokumar, “Cosmological model universe consisting of two forms of dark energy,”
*International Journal of Theoretical Physics*, vol. 53, no. 12, pp. 4360–4365, 2014. View at Publisher · View at Google Scholar - K. M. Singh and K. L. Mahanta, “Do neutrinos contribute to total dark energy,”
*Astrophysics and Space Science*, vol. 361, no. 85, 2016. View at Publisher · View at Google Scholar - K. Bamba, “Thermodynamic properties of modified gravity theories,”
*International Journal of Geometric Methods in Modern Physics*, vol. 13, no. 6, Article ID 1630007, 2016. View at Publisher · View at Google Scholar · View at MathSciNet - M. Zubair, M. Syed, and G. Abbas, “Bianchi type I and V solutions in f(R, T) gravity with time-dependent deceleration parameter,”
*Canadian Journal of Physics*, vol. 94, no. 12, pp. 1289–1296, 2016. View at Publisher · View at Google Scholar - S. D. Maharaj, R. Goswami, S. V. Chervon, and A. V. Nikolaev, “Exact solutions for scalar field cosmology in gravity,”
*Modern Physics Letters A*, vol. 32, no. 30, Article ID 1750164, 2017. View at Publisher · View at Google Scholar - K. Priyokumar, K. M. Singh, and M. R. Mollah, “Whether lyra’s manifold itself is ahidden source of dark energy,”
*International Journal of Theoretical Physics*, vol. 56, no. 8, pp. 2607–2621, 2017. View at Publisher · View at Google Scholar - G. C. Samanta and R. Myrzakulov, “Imperfect fluid cosmological model in modified gravity,”
*Chinese Journal of Physics*, vol. 55, no. 3, pp. 1044–1054, 2017. View at Publisher · View at Google Scholar - J. P. M. Graça, G. I. Salako, and V. B. Bezerra, “Quasinormal modes of a black hole with a cloud of strings in einstein–gauss–bonnet gravity,”
*International Journal of Modern Physics D*, vol. 26, no. 10, Article ID 1750113, 2017. View at Publisher · View at Google Scholar - K. Bamba, S. D. Odintsov, and E. N. Saridakis, “Inflationary cosmology in unimodular F(T) gravity,”
*Modern Physics Letters A*, vol. 32, no. 21, Article ID 1750114, 2017. View at Publisher · View at Google Scholar - I. Noureen and M. Zubair, “Axially symmetric shear-free fluids in
*f(R, T)*gravity,”*International Journal of Modern Physics D: Gravitation, Astrophysics, Cosmology*, vol. 26, no. 11, Article ID 1750128, 17 pages, 2017. View at Publisher · View at Google Scholar · View at MathSciNet - G. C. Samanta, R. Myrzakulov, and P. Shah, “Kaluza–Klein bulk viscous fluid cosmological models and the validity of the second law of thermodynamics in f(R,T) gravity,”
*Zeitschrift für Naturforschung A*, vol. 72, no. 4, pp. 365–374, 2017. View at Publisher · View at Google Scholar - E. H. Baffou, M. J. Houndjo, M. Hamani-Daouda, and F. G. Alvarenga, “Late-time cosmological approach in mimetic f(R, T) gravity,”
*The European Physical Journal C*, vol. 77, p. 708, 2017. View at Publisher · View at Google Scholar - H. Azmat, M. Zubair, and I. Noureen, “Dynamics of shearing viscous fluids in gravity,”
*International Journal of Modern Physics D: Gravitation, Astrophysics, Cosmology*, vol. 27, no. 1, Article ID 1750181, 2018. View at Publisher · View at Google Scholar - J. K. Singh, R. Nagpal, and S. K. Pacif, “Statefinder diagnostic for modified Chaplygin gas cosmology in gravity with particle creation,”
*International Journal of Geometric Methods in Modern Physics*, vol. 15, no. 3, Article ID 1850049, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - S. D. Odintsov and V. K. Oikonomou, “Early-time cosmology with stiff era from modified gravity,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 96, no. 10, Article ID 104059, 2017. View at Publisher · View at Google Scholar · View at MathSciNet - A. Addazi, “Evaporation/antievaporation and energy conditions in alternative gravity,”
*International Journal of Modern Physics A*, vol. 33, no. 4, Article ID 1850030, 15 pages, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - H. Shabani and A. H. Ziaie, “Interpretation of f(R,T) gravity in terms of a conserved effective fluid,”
*International Journal of Modern Physics A*, vol. 33, no. 8, Article ID 1850050, 2018. View at Publisher · View at Google Scholar - S. D. Odintsov and V. K. Oikonomou, “Reconstruction of slow-roll
*F(R)*gravity inflation from the observational indices,”*Annals of Physics*, vol. 388, pp. 267–275, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - M. Zubair, H. Azmat, and I. Noureen, “Anisotropic stellar filaments evolving under expansion-free condition in f(R,T) gravity,”
*International Journal of Modern Physics D*, vol. 27, no. 4, Article ID 1850047, 2018. View at Publisher · View at Google Scholar - K. Kleidis and V. K. Oikonomou, “Scalar field assisted gravity inflation,”
*International Journal of Geometric Methods in Modern Physics*, vol. 15, no. 8, Article ID 1850137, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - R. K. Tiwari, A. Beesham, and B. Shukla, “Cosmological model with variable deceleration parameter in
*f(R, T)*modified gravity,”*International Journal of Geometric Methods in Modern Physics*, vol. 15, no. 7, Article ID 1850115, p. 10, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - S. Hansraj and A. Banerjee, “Dynamical behavior of the Tolman metrics in gravity,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 97, no. 10, Article ID 104020, 2018. View at Publisher · View at Google Scholar · View at MathSciNet - D. Rowland and I. B. Whittingham, “Models of interacting dark energy,”
*Monthly Notices of the Royal Astronomical Society*, vol. 390, no. 4, pp. 1719–1726, 2008. View at Publisher · View at Google Scholar - W. Cui, S. Borgani, and M. Baldi, “The halo mass function in interacting dark energy models,”
*Monthly Notices of the Royal Astronomical Society*, vol. 424, no. 2, pp. 993–1005, 2012. View at Publisher · View at Google Scholar - M. Baldi, “Clarifying the effects of interacting dark energy on linear and non-linear structure formation processes,”
*Monthly Notices of the Royal Astronomical Society*, vol. 414, no. 1, pp. 116–128, 2011. View at Publisher · View at Google Scholar - J. Sadeghi, M. Khurshudyan, A. Movsisyan, and H. Farahani, “Interacting ghost dark energy models with variable G and Λ,”
*Journal of Cosmology and Astroparticle Physics*, vol. 12, p. 31, 2013. View at Publisher · View at Google Scholar - M. Khurshudyan, E. Chubaryan, and B. Pourhassan, “Interacting quintessence models of dark energy,”
*International Journal of Theoretical Physics*, vol. 53, no. 7, pp. 2370–2378, 2014. View at Publisher · View at Google Scholar - O. Bertolami, F. Gil Pedro, and M. Le Delliou, “Dark energy-dark matter interaction and putative violation of the equivalence principle from the Abell cluster A586,”
*Physics Letters B*, vol. 654, no. 5-6, pp. 165–169, 2007. View at Publisher · View at Google Scholar · View at Scopus - G. Olivares, F. Atrio-Barandela, and D. Pavón, “Observational constraints on interacting quintessence models,”
*Physical Review D: Particles, Fields, Gravitation and Cosmology*, vol. 71, no. 6, Article ID 063523, pp. 1–7, 2005. View at Publisher · View at Google Scholar · View at Scopus - N. Bilic, G. B. Tupper, and R. D. Viollier, “Unification of dark matter and dark energy: the inhomogeneous Chaplygin gas,”
*Physics Letters B*, vol. 535, pp. 17–21, 2002. View at Publisher · View at Google Scholar