Advances in High Energy Physics
Volume 2019 (2019), Article ID 4026856, 8 pages
https://doi.org/10.1155/2019/4026856

Research Article

Phantom-Like Behavior in Modified Teleparallel Gravity

Sakineh Karimzadeh1,2 and Raheleh Shojaee³

¹Department of Physics, Faculty of Basic Sciences, University of Mazandaran, P.O. Box 47416-95447, Babolsar, Iran
²Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), P. O. Box 55134-441, Maragha, Iran
³Department of Physics, Azarbaijan Shahid Madani University, P.O. Box 53714-161, Tabriz, Iran

Correspondence should be addressed to Raheleh Shojaee; r.shojaee@azaruniv.ac.ir

Received 18 October 2018; Revised 18 January 2019; Accepted 4 February 2019; Published 20 March 2019

Academic Editor: Sunny Vagnozzi

Copyright © 2019 Sakineh Karimzadeh and Raheleh Shojaee. 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.

Abstract.

The recent data from Planck2018 shows that the equation of state parameter of effective cosmic fluid today is . This indicates that it is possible for the universe to be in a phantom dominated era today. While a phantom field is essentially capable of explaining this observation, it suffers from some serious problems such as instabilities and violation of the null energy condition. So, it would be interesting to realize this effective phantom behavior without adopting a phantom field. In this paper, we study possible realization of an effective phantom behavior in modified teleparallel gravity. We show that modified teleparallel gravity is able essentially to realize an effective phantom-like behavior in the absence of a phantom field. For this purpose, we choose some observationally viable functions and prove that there are some subspaces of the models parameter space capable of realizing a phantom-like behavior without adopting a phantom field.

1. Introduction

Different cosmological observations of the last two decades such as measurements of luminosity distances of Supernova Type Ia (SNIa) [1, 2], the cosmic microwave background (CMB) temperature anisotropy through the Wilkinson Microwave Anisotropy probe (WMAP) satellite [3–5], large scale structure [6], the integrated Sachs-Wolfe effect [7], and more recently the Planck satellite data [8, 9] show that the universe is currently in a positively accelerating phase of expansion. Since general relativity with ordinary matter and energy components cannot explain such a novel observation, different solutions have been proposed to justify this late time cosmic speed-up. There are generally two approaches to explain this observation by modification of Einstein’s field equations. The first approach attempts to modify the energy momentum (matter) part of the field equations by adding a yet unknown component dubbed dark energy, and the second approach tries to modify the geometric part of the field equations. Scalar fields dark energy models [10–12] belong to the first category, while modified gravity theories such as gravity [13, 14], Gauss-Bonnet and gravity [15, 16], massive gravity [17], Lovelock gravity [18], extra-dimensional gravity [19, 20], Teleparallel Equivalent of General Relativity (TEGR) [21–25], and gravity [26–28] belong to the second category. A simple candidate for dark energy proposal is the cosmological constant [29, 30] and the corresponding cosmological model (the CDM) has very good agreement with recent observational data. But this scenario has not a dynamical behavior and its equation of state parameter stays always at . The origin of cosmological constant is not yet well understood; it needs a huge amount of fine-tuning and it is impossible to realize phantom divide line crossing in the pure CDM model. Because of these shortcomings with cosmological constant, in recent years attention has been drawn towards modified gravity theories and, among the various kinds of modified gravity models, teleparallel gravity (TEGR) and gravity have recently obtained a lot of regard. Teleparallel gravity is completely equivalent to general relativity at the level of equations and in this theory the Lagrangian is written in terms of the torsion scalar . Much similar to the gravity that one replaces by in the Einstein-Hilbert action of general relativity, gravity is an extension of TEGR that replaces by a generic function of torsion as in teleparallel gravity. In this model the Ricci scalar is zero since there is no curvature; instead the torsion field is considered in the framework of Einstein’s other (teleparallel) gravity. In recent years, various aspects of teleparallel and modified teleparallel gravity are studied in details (see [31–37] for some various works in this field). The observational viability of teleparallel and modified teleparallel gravity has been studied in [38, 39].

With an effective phantom-like behavior one means that the effective energy density of the cosmic fluid is positive and increases with time, and at the same time the effective equation of state parameter stays less than [40]. Typically for realization of such a behavior phantom fields are considered, while the existence of phantom field causes instabilities and violates the null energy condition [41–43]. Possible realization of phantom-like behavior in some cosmological models such as the DGP braneworld model [44–46] and gravity is studied [47]. Also possible existence of a phantom-like phase in teleparallel and also modified teleparallel gravity theories have been studied in some references such as = [28, 48–51]. In this paper, we study possible realization of the phantom-like behavior in modified teleparallel, , gravity. In order to achieve this goal, we choose three viable models of gravity and, with appropriate selection of the models parameters, we show that phantom-like behavior can be realized without any phantom fields in these models of modified teleparallel gravity. This result is important because unlike phantom fields, gravity respects the null energy condition and, more importantly, matter is always stable in this framework [52]. The paper is organized as follows. In Section 2, we briefly review field equations in gravity. In Section 3, we choose three models of in order to see whether the adopted models have an effective phantom behavior or not. For this purpose, we plot the effective energy density and the equation of state parameter versus the redshift and compare the results with the latest observational data from Planck2018. Finally, in Section 4, we present the summary and conclusion.

2. Field Equations for Modified Teleparallel Gravity

2.1. Field Equations of Gravity

In teleparallel (Einstein’s other) gravity one needs to define four orthogonal vector fields named tetrads which form a basis for spacetime manifold. In this framework, the manifold and the Minkowski metrics are related as follows [21, 52]:

where the Greek indices run from to in coordinate basis of the manifold while the Latin indices run the same but in the tangent space of the manifold and is the Minkowski metric. The connection in teleparallel gravity, that is, the Weitzenbock connection, is defined as follows:

which gives the spacetime a nonzero torsion but zero curvature in contrast to general relativity. By this definition the torsion tensor and its permutations are

where is called the Superpotential. In correspondence with Ricci scalar we define a torsion scalar as

So, the gravitational action of teleparallel gravity can be written as follows:

where is the determinant of the vierbein which is equal to . Variation of this action with respect to the vierbeins gives the teleparallel field equations as follows:

Now similar to modifying the action of general relativity in which is replaced by a general function , one can replace the teleparallel action by a function . Doing this, the resulting modified field equations are

where is the energy momentum tensor of matter, , and . We note that we have set the spin connection to zero (as usually it is done in the formulation of gravity). In this case the theory does not have local Lorentz invariance. In what follows we set .

2.2. Cosmological Considerations

Now for cosmological considerations we assume a spatially flat FRW metric as [34, 53]

where is the scale factor of the universe. For Lagrangian density, we obtain

where is the Hubble parameter. Therefore, the cosmological field equations become

and

where and are the ordinary matter energy density and pressure, respectively. The conservation equation in this framework is as follows:

Now, (12) and (13) can be rewritten as follows:

and

where and are the energy density and pressure of the torsion fluid that are defined as follows, respectively,

Finally, the equation of state parameter of the torsion fluid, , is defined as

Note that if we consider , then (17) and (19) can be rewritten as follows:

respectively. With these preliminaries, in the next section we study possible realization of the phantom-like behavior in some observationally viable models.

3. Phantom-Like Behavior in Gravity

To have an effective phantom-like behavior, the effective energy density must be positive and growing positively with time. Also the equation of state parameter should be less than . It has been shown that modifying the geometric part of the Einstein field equations alone leads to an effective phantom-like behavior while there is no phantom field in the problem (see [44–47]). Now we show that modified teleparallel gravity ( gravity) can realize an effective phantom-like behavior while the null energy condition for the effective cosmic (torsion) fluid, that is, , is respected. We note that as has been shown in [52], matter is always stable in these theories. To see the phantom-like behavior of gravity, we adopt some models of gravity that could be viable through, for instance, cosmological and solar system tests. In this respect we consider a scale factor of the type

This scale factor has two adjustable parameters, and , and by assumption . This choice is coming from bouncing cosmological solutions in the context of string theory with quintom matter [54]. Note that this choice belongs to the class of scale factors that are usually adopted in literature. Based on the definition , with this choice of the scale factor and (11), we find

We note that it is easy to show that the scale factor (22) with two adjustable parameters, and , is essentially a solution of the field equations. So, in what follows we explore possible realization of the effective phantom-like behavior with adopted functions.

3.1. Phantom-Like Effect with

In this form of , and are two model’s dimensionless parameters, in which only is an independent parameter. As we can see, for , this type of gravity can reduce to cosmology, while for it reduces to the Dvali, Gabadadze, and Porrati (DGP) braneworld model. Inserting into the first Friedmann equation (12) and calculating the result for the present time, we obtain as follows [34]:

where and are the dimensionless density parameter of the dust matter and the present Hubble parameter, respectively. We note that, in order to have a positively accelerating expansion of the universe, we need those values of , where [55]. Now for this type of gravity, we find that (remember that )

and

By applying (20) and (21), we obtain the effective density and equation of state parameter for this model as

Now to see whether this model has an effective phantom-like behavior or not, we plot the evolution of the effective energy density and the equation of state parameter versus the redshift, . In this manner we obtain a suitable amount for the independent parameter to have an effective phantom-like behavior that this amount is about . In this respect, by using the equations (28) and (29), Figures 1 and 2 are plotted. Also we have used , , and in all numerical calculations in the paper. This value is in agreement with the results reported in literature. In Figure 2, as we can see the effective equation of state parameter for the present time () is ; this amount is in favor of the recent data from Planck2018. However, we should pay attention that, in this form of , the effective equation of state parameter crosses the cosmological constant (phantom divide) line, , from phantom-like phase to the quintessence-like phase in future. This behavior is not in favor of the observational data that show transition from the quintessence phase to the phantom phase. Nevertheless, having a positively growing energy density is a favorable capability of this model.

Figure 1: Variation of the effective energy density versus the redshift for .

Figure 2: Variation of effective equation of state parameter versus the redshift for , where the dash lines represent .

3.2. Phantom-Like Effect with

In this model is an independent parameter and is the current value of the torsion scalar. In the limit , this model recovers the model [34]. Also, by using the modified Friedmann equation, we find

In this model, if the universe has a phantom phase (with ) and if it has a quintessence phase (with ) [48]. For this form of function we obtain

and

Once again, using (20) and (21) we acquire and in the present model as follows:

and

respectively. We try to see possible realization of the effective phantom-like behavior in this model by numerical treatment of these quantities. We investigated the behavior of and versus the redshift, , for different choices of the model parameter . Our analysis shows that the phase of expansion of the universe (according to the values of ) depends on the sign of the parameter . We find that is the acceptable value for realization of an effective phantom-like behavior in this model. By using (34) and (35), the evolutions of and versus the redshift are shown, respectively, in Figures 3 and 4. Figure 3 shows an increasing (positively growing) energy density with the cosmic time (inverse of the redshift). In Figure 4, as we can see with the proper selection of parameters, this model can display for present time. Also Figure 4 shows that the effective equation of state stays always less than in this model. Therefore, we note that in this model the crossing of the phantom divide could not occur and the universe evermore is in the phantom phase. Similar to the previous case, this behavior is not in favor of the observational data that shows transition from the quintessence phase to the phantom phase. Therefore, we can conclude that the present model is not observationally viable.

Figure 3: Variation of the effective energy density versus the redshift for .

Figure 4: Variation of effective equation of state parameter versus the redshift for , where the dash lines represent .

3.3. Phantom-Like Effect with

The above two models have been used in the literatures for a variety of purposes. Possible transition to the phantom phase of the cosmic expansion has been treated with the mentioned models in a context a little different from our approach. Here and for the sake of more novelty of the treatment, we consider a combined model that contains a relatively more general function. This approach is introduced in [48]. The number of free parameters here is more than the previous cases. Usually with a wider parameter space one expects to encounter more fine-tuning of the parameter to have cosmologically viable solutions. But, in the same time it is easier, in principle, to find some subspaces of the model parameter space to fulfill the required expectation. For the sake of simplicity, we have taken and . Here and are two parameters of model; only is free parameter because can be obtained as

Also for this combined model, we can acquire

and

Similar to the former two models, by using (20) and (21) we obtain the effective density and equation of state parameter for this model respectively as follows:

and

where we have defined

and

Finally, to investigate the possible realization of the phantom-like behavior in this combined model, by using (40) and (41), we plot and versus the redshift for different values of . We observe that the two conditions for effective phantom mimicry, (a) where the effective energy density must be positive and growing with time (b) the equation of state parameter should be less than , are satisfied if . This typical behavior of and versus the redshift is shown in Figures 5 and 6, respectively. We note that unlike the previous two cases, this model is strictly in favor of the observational data. As is seen from Figure 6, it is obvious that the effective equation of state parameter can cross the line at and amount for current time () is consistent with the resent observational data. It means that universe evolves from quintessence-like phase towards the phantom-like phase. We can conclude that this model is capable of realizing a suitable dynamical mechanism for getting the present time cosmic acceleration and transition to a phantom-like stage in a fascinating manner. Consequently, this model is more cosmologically viable than the previous two models.

Figure 5: Variation of the effective energy density versus the redshift for .

Figure 6: Variation of effective equation of state parameter versus the redshift for , where the dash lines represent .

4. Conclusion

In this paper, we have investigated possible realization of an effective phantom behavior in some viable gravity models. With effective phantom-like behavior we mean an effective energy density that should be positive and growing positively with time and, also, the equation of state parameter should be less than . We have chosen three different models of gravity where two of them are reliable based on previous studies and our third model is a combined model. We have shown that model with realizes an effective phantom-like behavior if . As is shown in Figure 2, we obtained the effective equation of state parameter for present time about , where this amount is acceptable according to the recent data from Planck2018. But, this model evolves from effective phantom-like phase towards the effective quintessence-like phase in future. Thus, this model is not in complete favor of observation, since observation shows transition from quintessence-like to phantom-like phase. We have presented another model, which is . This model realizes an effective phantom-like behavior if . Although is obtained as an acceptable value that is shown in Figure 4, this function is not also in favor of observation, since in this model the crossing of the phantom divide could not occur and the universe evermore is in the phantom phase. Finally, we have constructed a theory by combining the two previous models, where it only contains one model parameter . This model realizes an effective phantom-like behavior if . Unlike the previous two models, this model is cosmologically more viable, since the equation of state parameter in this model evolves from effective quintessence-like phase towards an effective phantom-like phase. As is shown in Figure 6, it is obvious that can cross the line at and amount is consistent with the resent observational data. Therefore, this combined model is in agreement with the observational data.

Data Availability

The data used to support the findings of this study are included within the article.

Conflicts of Interest

The authors declare that they have no conflicts of interest.

Acknowledgments

It is a pleasure to thank Professor Kourosh Nozari for helpful discussions and valuable comments. Also this work has been supported financially by Research Institute for Astronomy and Astrophysics of Maragha (RIAAM) under research project number 1/6025-64.

References

S. Perlmutter, G. Aldering, and G. Goldhaber, “Measurements of and from 42 high-redshift supernovae,” The Astrophysical Journal, vol. 517, no. 2, pp. 565–586, 1999.

A. G. Riess, L.-G. Sirolger, J. Tonry et al., “Type Ia supernova discoveries at z>1 from the Hubble Space Telescope: evidence for past deceleration and constraints on dark energy evolution,” The Astrophysical Journal, vol. 607, no. 2, pp. 665–687, 2004.

G. Hinshaw, C. Barnes, C. L. Bennett et al., “Three-year wilkinson microwave anisotropy probe (WMAP) observations: temperature analysis,” The Astrophysical Journal Supplement Series, 2007.

G. Hinshaw, D. Larson, E. Komatsu et al., “Nine-year wilkinson microwave anisotropy probe (WMAP) observations: cosmological parameter results,” Astrophysics: Cosmology and Nongalactic Astrophysics, 2012.

C. L. Bennett, D. Larson, J. L. Weiland et al., “Nine-year wilkinson microwave anisotropy probe (WMAP) observations: final maps and results,” Astrophysics: Cosmology and Nongalactic Astrophysics, 2012.

M. Tegmark, M. Strauss, M. Blanton et al., “Cosmological parameters from SDSS and WMAP,” Physical Review D: Particles, Fields, Gravitation, and Cosmology, Article ID 103501, 2004.

S. P. Boughn and R. G. Crittenden, “A detection of the integrated Sachs-Wolfe effect,” New Astronomy Reviews, vol. 49, no. 2, pp. 75–78, 2005.

P. A. R. Ade, N. Aghanim, C. Armitage-Caplan et al., “Planck 2013 results. XVI. Cosmological parameters,” Astrophysics: Cosmology and Nongalactic Astrophysics, 2013.

N. Aghanim, Y. Akrami, M. Ashdown et al., “Planck 2018 results. VI. Cosmological parameters,” Astrophysics: Cosmology and Nongalactic Astrophysics, 2018.

J. Weller, “Bubbles from dark energy?” Astrophysics, 2000.

E. J. Copeland, M. Sami, and S. Tsujikawa, “Dynamics of dark energy,” International Journal of Modern Physics D: Gravitation, Astrophysics, Cosmology, vol. 15, no. 11, pp. 1753–1935, 2006.

Y. F. Cai, E. N. Saridakis, M. R. Setare, and J. Xia, “Quintom cosmology: theoretical implications and observations,” Physics Reports, vol. 493, no. 1, pp. 1–60, 2010.

A. De Felice and S. J. Tsujikawa, “f(R) theories,” Living Reviews in Relativity, vol. 13, p. 3, 2010.

S. Nojiri and S. D. Odintsov, “Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models,” Physics Reports, vol. 505, pp. 59–144, 2011.

S. Nojiri and S. D. Odintsov, “Modified Gauss–Bonnet theory as gravitational alternative for dark energy,” Physics Letters B, vol. 631, no. 1-2, pp. 1–6, 2005.

A. De Felice and S. Tsujikawa, “Construction of cosmologically viable f(G) dark energy models,” Physics Letters B, vol. 675, no. 1, pp. 1–8, 2009.

C. de Rham, “Massive gravity,” Living Reviews in Relativity, vol. 17, no. 7, 2014.

N. Deruelle and L. Fariña-Busto, “Lovelock gravitational field equations in cosmology,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 41, no. 12, pp. 3696–3708, 1990.

P. Hořava, “Membranes at quantum criticality,” Journal of High Energy Physics, vol. 2009, article 020, 2009.

K. Nozari, “DGP cosmology with a non-minimally coupled scalar field on the brane,” Journal of Cosmology and Astroparticle Physics, no. 9, 2007.

K. Hayashi and T. Shirafuji, “New general relativity,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 19, no. 12, pp. 3524–3553, 1979.

A. Unzicker and T. Case, “Translation of Einsteins attempt of a unified field theory with teleparallelism,” History and Philosophy of Physics, 2005.

G. Y. Chee, Y. Zhang, and Y. Guo, “Gravitational energy-momentum and the Hamiltonian formulation of the teleparallel gravity,” General Relativity and Quantum Cosmology, 2001.

R. Aldrovandi and J. G. Pereira, Teleparallel Gravity: An Introduction, vol. 173, Springer, New York, NY, USA, 2013.

J. W. Maluf, “The teleparallel equivalent of general relativity,” Annalen der Physik, vol. 525, no. 5, pp. 339–357, 2013.

G. R. Bengochea and R. Ferraro, “Dark torsion as the cosmic speed-up,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 79, no. 12, Article ID 124019, 5 pages, 2009.

P. Wu and H. Yu, “The dynamical behavior of f(T) theory,” Physics Letters B, vol. 692, pp. 176–179, 2010.

J. B. Dent, S. Dutta, and E. N. Saridakis, “f(T) gravity mimicking dynamical dark energy. Background and perturbation analysis,” Journal of Cosmology and Astroparticle Physics, vol. 2011, 2011.

S. M. Carroll, “The cosmological constant,” Living Reviews in Relativity, vol. 4, article 1, 2001.

T. Padmanabhan, “Cosmological constant—the weight of the vacuum,” Physics Reports, vol. 380, no. 5-6, pp. 235–320, 2003.

K. Nozari, R. Shojaee, and S. Karimzadeh, “Interpretation of rotation curves of spiral galaxies in modified teleparallel gravity,” Communications in Theoretical Physics, vol. 60, no. 6, pp. 687–690, 2013.

A. Behboodi, S. Akhshabi, and K. Nozari, “Braneworld setup and embedding in teleparallel gravity,” Physics Letters. B. Particle Physics, Nuclear Physics and Cosmology, 2014.

F. Kiani and K. Nozari, “Energy conditions in F(T, Θ) gravity and compatibility with a stable de Sitter solution,” Physics Letters B, 2014.

Y.-F. Cai, S. Capozziello, M. De Laurentis, and E. N. Saridakis, “F(T) teleparallel gravity and cosmology,” Reports on Progress in Physics, vol. 79, no. 04, 2016.

R. C. Nunes, “Structure formation in gravity and a solution for tension,” Journal of Cosmology and Astroparticle Physics, vol. 05, no. 052, 2018.

G. G. L. Nashed and E. N. Saridakis, “Rotating AdS black holes in Maxwell-f(T)gravity,” High Energy Physics - Theory, 2018.

U. Debnath, “Charge gravastars in f(T) modified gravity,” General Relativity and Quantum Cosmology, 2019.

R. C. Nunes, S. Pan, and E. N. Saridakis, “New observational constraints on f(T) gravity from cosmic chronometers,” Journal of Cosmology and Astroparticle Physics, vol. 2016, no. 08, article no. 011, 2016.

R. C. Nunes, A. Bonilla, S. Pan, and E. N. Saridakis, “Observational constraints on f(T) gravity from varying fundamental constants,” The European Physical Journal C, vol. 77, no. 4, 2017.

L. P. Chimento, R. Lazkoz, R. Maartens, and I. Quiros, “Crossing the phantom divide without phantom matter,” Journal of Cosmology and Astroparticle Physics, no. 9, 2006.

V. Sahni and Y. Shtanov, “Braneworld models of dark energy,” Journal of Cosmology and Astroparticle Physics, vol. 11, article 014, 2003.

V. Sahni, “Cosmological surprises from braneworld models of dark energy,” General relativity and Gravitation, 2005.

A. Lue and G. D. Starkman, “How a brane cosmological constant can trick us into thinking that w < -1,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 70, no. 10, pp. 1–101501, 2004.

K. Nozari and M. Pourghasemi, “Crossing the phantom divide line in a Dvali-Gabadadze-Porrati-inspired F(R,φ) gravity,” Journal of Cosmology and Astroparticle Physics, vol. 2008, no. 10, 2008.

K. Nozari and T. Azizi, “Phantom-like effects on warped DGP brane,” Communications in Theoretical Physics, vol. 54, no. 4, pp. 773–780, 2010.

K. Nozari and N. Alipour, “Phantom mimicry on the normal branch of a dgp-inspired braneworld scenario with curvature effect,” Modern Physics Letters A, vol. 25, no. 3, pp. 189–210, 2010.

K. Nozari and T. Azizi, “Phantom-Like in f(R) Gravity,” Physics Letters B, vol. 608, no. 205, 2009.

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, no. 1, 2011.

R.-J. Yang, “New types of gravity,” The European Physical Journal C, vol. 71, Article ID 1797, 2011.

P. Wu and H. Yu, “Observational constraints on f(T) theory,” Physics Letters B, 2010.

C.-Q. Geng, C.-C. Lee, E. N. Saridakis, and Y.-P. Wu, “‘Teleparallel’ dark energy,” Physics Letters B, vol. 704, no. 5, pp. 384–387, 2011.

A. Behboodi, S. Akhshabi, and K. Nozari, “Matter stability in modified teleparallel gravity,” Physics Letters B, vol. 718, no. 30, 2012.

A. Paliathanasis, J. D. Barrow, and P. G. Leach, “Cosmological solutions of gravity,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 94, no. 2, Article ID 023525, 10 pages, 2016.

Y.-F. Cai, T. Qiu, Y.-S. Piao, M. Li, and X. Zhang, “Bouncing universe with quintom matter,” Journal of High Energy Physics, vol. 0710, no. 071, 2007.

S. Nesseris, S. Basilakos, E. N. Saridakis, and L. Perivolaropoulos, “Viable f(T) models are practically indistinguishable from LCDM,” Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 88, no. 10, Article ID 103010, 2013.