# Phantom-Like Behavior in Modified Teleparallel Gravity

Authors: Sakineh Karimzadeh; Raheleh Shojaee
Journal: Advances in High Energy Physics
 (2019)

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## Abstract

The recent data from Planck2018 shows that the equation of state parameter of effective cosmic fluid today isw0=-1.03±0.03. 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 f(T) 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.


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## Body

## 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 f(R) gravity [13, 14], Gauss-Bonnet and f(G) gravity [15, 16], massive gravity [17], Lovelock gravity [18], extra-dimensional gravity [19, 20], Teleparallel Equivalent of General Relativity (TEGR) [21–25], and f(T) 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 ΛCDM) 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 -1. 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 ΛCDM 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 f(T) 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 T. Much similar to the f(R) gravity that one replaces R by f(R) in the Einstein-Hilbert action of general relativity, f(T) gravity is an extension of TEGR that replaces T by a generic function of torsion as f(T) in teleparallel gravity. In this model the Ricci scalar R 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 aneffective 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 -1 [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 f(R) 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, f(T), gravity. In order to achieve this goal, we choose three viable models of f(T) 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, f(T) 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 f(T) gravity. In Section 3, we choose three models of f(T) 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 z 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 off(T) Gravity

In teleparallel (Einstein’s other) gravity one needs to define four orthogonal vector fields namedtetrads which form a basis for spacetime manifold. In this framework, the manifold and the Minkowski metrics are related as follows [21, 52]:(1)gμν=ηijeμieνj, where the Greek indices run from 0 to 3 in coordinate basis of the manifold while the Latin indices run the same but in the tangent space of the manifold and ηij=diag(+1,-1,-1,-1) is the Minkowski metric. The connection in teleparallel gravity, that is, the Weitzenbock connection, is defined as follows:(2)Γρμν=eiρ∂νeμi, 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(3)Tρμν≡eiρ∂μeνi-∂νeμi(4)Kμνρ=-12Tμνρ-Tνμρ-Tρμν(5)Sρμν=12Kμνρ+δρμTανα-δρνTαμα,where Sρμν is called theSuperpotential. In correspondence with Ricci scalar we define a torsion scalar as(6)T=SρμνTρμν. So, the gravitational action of teleparallel gravity can be written as follows:(7)I=116πG∫d4xeT, where e≡det⁡(eμα)=-det⁡(gμν) is the determinant of the vierbein eμa which is equal to -g. Variation of this action with respect to the vierbeins gives the teleparallel field equations as follows:(8)e-1∂μeeiρSρμν-eiλTρμλSρνμ+14eiνT=4πGeiρΘρν. Now similar to modifying the action of general relativity in which R is replaced by a general function f(R), one can replace the teleparallel action T by a function f(T). Doing this, the resulting modified field equations are (9)e-1∂μeSiμνfTT-eiλTρμλSρνμfTT+Siμν∂μTfTTT+14eiνfT=4πGeiρΘρν,where Θρν is the energy momentum tensor of matter, fT≡df/dT, and fTT≡d2f/dT2. We note that we have set the spin connection to zero (as usually it is done in the formulation of f(T) gravity). In this case the theory does not have local Lorentz invariance. In what follows we set 4πG=1.


### 2.2. Cosmological Considerations

Now for cosmological considerations we assume a spatially flat FRW metric as [34, 53](10)eμα=diag⁡1,-at,-at,-at, where a(t) is the scale factor of the universe. For Lagrangian density, we obtain(11)T=-6a˙a2=-6H2, where H=a˙/a is the Hubble parameter. Therefore, the cosmological field equations become(12)12H2fTT+fT=16πGρ, and(13)48H2H˙fTTT-4H˙+3H2fTT-fT=16πGρ, where ρ and p are the ordinary matter energy density and pressure, respectively. The conservation equation in this framework is as follows:(14)ρ˙+3Hρ+p=0. Now, (12) and (13) can be rewritten as follows:(15)H2=16πG3ρ+ρT, and(16)2H˙+3H2=-8πGP+PT, where P(T) and ρ(T) are the energy density and pressure of thetorsion fluid that are defined as follows, respectively,(17)ρT=2TfTT-fT-T16πG,(18)PT=4H˙2TfTTT+fTT-1-ρT16πG.Finally, the equation of state parameter of the torsion fluid, ω(T), is defined as(19)ωT≡PTρT=-1+4H˙2TfTTT+fTT-12TfTT-fT-T. Note that if we consider f(T)=T+F(T), then (17) and (19) can be rewritten as follows:(20)ρT=2TFT-F16πG,(21)ωT=-1+F-2TFT-TFT+2TFTT1+FT+2TFTTF-2TFT,respectively. With these preliminaries, in the next section we study possible realization of the phantom-like behavior in some observationally viable f(T) models.


## 2.1. Field Equations off(T) Gravity

In teleparallel (Einstein’s other) gravity one needs to define four orthogonal vector fields namedtetrads which form a basis for spacetime manifold. In this framework, the manifold and the Minkowski metrics are related as follows [21, 52]:(1)gμν=ηijeμieνj, where the Greek indices run from 0 to 3 in coordinate basis of the manifold while the Latin indices run the same but in the tangent space of the manifold and ηij=diag(+1,-1,-1,-1) is the Minkowski metric. The connection in teleparallel gravity, that is, the Weitzenbock connection, is defined as follows:(2)Γρμν=eiρ∂νeμi, 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(3)Tρμν≡eiρ∂μeνi-∂νeμi(4)Kμνρ=-12Tμνρ-Tνμρ-Tρμν(5)Sρμν=12Kμνρ+δρμTανα-δρνTαμα,where Sρμν is called theSuperpotential. In correspondence with Ricci scalar we define a torsion scalar as(6)T=SρμνTρμν. So, the gravitational action of teleparallel gravity can be written as follows:(7)I=116πG∫d4xeT, where e≡det⁡(eμα)=-det⁡(gμν) is the determinant of the vierbein eμa which is equal to -g. Variation of this action with respect to the vierbeins gives the teleparallel field equations as follows:(8)e-1∂μeeiρSρμν-eiλTρμλSρνμ+14eiνT=4πGeiρΘρν. Now similar to modifying the action of general relativity in which R is replaced by a general function f(R), one can replace the teleparallel action T by a function f(T). Doing this, the resulting modified field equations are (9)e-1∂μeSiμνfTT-eiλTρμλSρνμfTT+Siμν∂μTfTTT+14eiνfT=4πGeiρΘρν,where Θρν is the energy momentum tensor of matter, fT≡df/dT, and fTT≡d2f/dT2. We note that we have set the spin connection to zero (as usually it is done in the formulation of f(T) gravity). In this case the theory does not have local Lorentz invariance. In what follows we set 4πG=1.


## 2.2. Cosmological Considerations

Now for cosmological considerations we assume a spatially flat FRW metric as [34, 53](10)eμα=diag⁡1,-at,-at,-at, where a(t) is the scale factor of the universe. For Lagrangian density, we obtain(11)T=-6a˙a2=-6H2, where H=a˙/a is the Hubble parameter. Therefore, the cosmological field equations become(12)12H2fTT+fT=16πGρ, and(13)48H2H˙fTTT-4H˙+3H2fTT-fT=16πGρ, where ρ and p are the ordinary matter energy density and pressure, respectively. The conservation equation in this framework is as follows:(14)ρ˙+3Hρ+p=0. Now, (12) and (13) can be rewritten as follows:(15)H2=16πG3ρ+ρT, and(16)2H˙+3H2=-8πGP+PT, where P(T) and ρ(T) are the energy density and pressure of thetorsion fluid that are defined as follows, respectively,(17)ρT=2TfTT-fT-T16πG,(18)PT=4H˙2TfTTT+fTT-1-ρT16πG.Finally, the equation of state parameter of the torsion fluid, ω(T), is defined as(19)ωT≡PTρT=-1+4H˙2TfTTT+fTT-12TfTT-fT-T. Note that if we consider f(T)=T+F(T), then (17) and (19) can be rewritten as follows:(20)ρT=2TFT-F16πG,(21)ωT=-1+F-2TFT-TFT+2TFTT1+FT+2TFTTF-2TFT,respectively. With these preliminaries, in the next section we study possible realization of the phantom-like behavior in some observationally viable f(T) models.


## 3. Phantom-Like Behavior inf(T) 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-1. 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 (f(T) gravity) can realize an effective phantom-like behavior while the null energy condition for the effective cosmic (torsion) fluid, that is, (ρ(T)+P(T)≥0), 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 f(T) gravity, we adopt some models of f(T) gravity that could be viable through, for instance, cosmological and solar system tests. In this respect we consider a scale factor of the type(22)at=t2+t01-ν1/1-ν. This scale factor has two adjustable parameters, t0 and ν, and by assumption ν≠1. 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 a(t)=a0tn that are usually adopted in literature. Based on the definition 1+z=1/a(t), with this choice of the scale factor and (11), we find(23)T=-241/1+z1-ν-t0/1-ν1+z21-ν1-ν2. We note that it is easy to show that the scale factor (22) with two adjustable parameters, t0 and ν, is essentially a solution of the field equations. So, in what follows we explore possible realization of the effective phantom-like behavior with adopted f(T) functions.


### 3.1. Phantom-Like Effect withf(T)=T+f0(-T)p

In this form off(T), f0 and p are two model’s dimensionless parameters, in which only p is an independent parameter. As we can see, for p=0, this type of f(T) gravity can reduce to ΛCDM cosmology, while for p=1/2 it reduces to the Dvali, Gabadadze, and Porrati (DGP) braneworld model. Inserting f(T)=T+f0(-T)p into the first Friedmann equation (12) and calculating the result for the present time, we obtain f0 as follows [34]:(24)f0=1-Ωm06H02p-12p-1, where Ωm0 and H0 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 p, where p<1 [55]. Now for this type of f(T) gravity, we find that (remember that f(T)≡T+F(T))(25)FT=f0-Tp,(26)FT=-f0p-Tp-1,and(27)FTT=f0pp-1-Tp-2. By applying (20) and (21), we obtain the effective density and equation of state parameter for this model as(28)ρT=f0-Tp2p-116πG(29)ωT=-1+pf0-Tp1-2p-pTpf0-Tp1-2p-T.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,z. In this manner we obtain a suitable amount for the independent parameter p to have an effective phantom-like behavior that this amount is about p=0.028. In this respect, by using the equations (28) and (29), Figures 1 and 2 are plotted. Also we have used Ωm0=0.315, H0=67.4kms-1Mpc-1, and ν=1.95 in all numerical calculations in the paper. This value p 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 (z=0) is ω0=-1.03; this amount is in favor of the recent data from Planck2018. However, we should pay attention that, in this form of f(T), the effective equation of state parameter crosses the cosmological constant (phantom divide) line, ω=-1, 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 forf(T)=T+f0(-T)p.Figure 2
Variation of effective equation of state parameter versus the redshift forf(T)=T+f0(-T)p, where the dash lines represent ω0(T)=-1.03.


### 3.2. Phantom-Like Effect withf(T)=T+ξT(1-eαT0/T)

In this modelα is an independent parameter and T0=T(z=0) is the current value of the torsion scalar. In the limit α→0, this model recovers the ΛCDM model [34]. Also, by using the modified Friedmann equation, we find(30)ξ=-1-Ωm01-1-2αeα. In this model, if α>0 the universe has a phantom phase (with ω<-1) and if α<0 it has a quintessence phase (with ω>-1) [48]. For this form of f(T) function we obtain(31)FT=ξT1-eαT0/T,(32)FT=ξαT0TeαT0/T+ξ1-eαT0/T,and(33)FTT=-α2T02ξT3eαT0/T. Once again, using (20) and (21) we acquire ρ(T) and ω(T) in the present model as follows:(34)ρT=2αξT0eαT0/T+Tξ1-eαT0/T16πG, and(35)ωT=-1+TξeαT0/T-1-2ξαT0eαT0/T-Tξ-ξeαT0/T1-αT0/T+2α2T02/T2TξeαT0/T-1-2ξαT0eαT0/Tξ-ξeαT0/T1-αT0/T+2α2T02/T2+1, 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 ρ(T) and ω(T) versus the redshift, z, for different choices of the model parameter α. Our analysis shows that the phase of expansion of the universe (according to the values of ω) depends on the sign of the parameter α. We find that α=0.07 is the acceptable value for realization of an effective phantom-like behavior in this model. By using (34) and (35), the evolutions of ρ(T) and ω(T) 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 ω(T)=-1.03 for present time. Also Figure 4 shows that the effective equation of state stays always less than -1 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 forf(T)=T+ξT(1-eαT0/T).Figure 4
Variation of effective equation of state parameter versus the redshift forf(T)=T+ξT(1-eαT0/T), where the dash lines represent ω0(T)=-1.03.


### 3.3. Phantom-Like Effect withf(T)=T+n(T-Te(βT0/T)+(-T)β)

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 mentionedf(T) 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 f(T) 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 ξ=f0≡n and p=α≡β. Here β and n are two parameters of model; only β is free parameter because n can be obtained as(36)n=-Ωm0-11-2β6H02β-2+1-1-2βeβ. Also for this combined model, we can acquire(37)FT=nT-TeβT0/T+-Tβ,(38)FT=nβT0TeβT0/T+n1-eβT0/T-nβ-Tβ-1,and(39)FTT=-nβ2T02T3eβT0/T+nββ-1-Tp-2. 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:(40)ρT=n-Tβ2β-1+T+eβT0/T2βT0-T16πG, and(41)ωT=-1+ΘΥ, where we have defined(42)Θ≡n-Tβ1-2β+eβT0/TTn-2nβT0-T1+n-Tn1-2β+eβT0/TT-2βT0-T and(43)Υ≡1+βT0/T-2β2T02/T2-1eβT0/T+1-2ββ-Tβ-11+nβT0/T-2β2T02/T2-1eβT0/T+n+nβ1-2β-Tβ-1.Finally, to investigate the possible realization of the phantom-like behavior in this combined model, by using (40) and (41), we plot ρ(T) and ω(T) versus the redshift for different values of β. 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 -1, are satisfied if β=0.2. This typical behavior of ρ(T) and ω(T) 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 ω(T)=-1 line at 0.5<zcross<1 and amount ω(T) for current time (z=0) 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 forf(T)=T+n(T-Te(βT0/T)+(-T)β).Figure 6
Variation of effective equation of state parameter versus the redshift forf(T)=T+n(T-Te(βT0/T)+(-T)β), where the dash lines represent ω0(T)=-1.03.


## 3.1. Phantom-Like Effect withf(T)=T+f0(-T)p

In this form off(T), f0 and p are two model’s dimensionless parameters, in which only p is an independent parameter. As we can see, for p=0, this type of f(T) gravity can reduce to ΛCDM cosmology, while for p=1/2 it reduces to the Dvali, Gabadadze, and Porrati (DGP) braneworld model. Inserting f(T)=T+f0(-T)p into the first Friedmann equation (12) and calculating the result for the present time, we obtain f0 as follows [34]:(24)f0=1-Ωm06H02p-12p-1, where Ωm0 and H0 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 p, where p<1 [55]. Now for this type of f(T) gravity, we find that (remember that f(T)≡T+F(T))(25)FT=f0-Tp,(26)FT=-f0p-Tp-1,and(27)FTT=f0pp-1-Tp-2. By applying (20) and (21), we obtain the effective density and equation of state parameter for this model as(28)ρT=f0-Tp2p-116πG(29)ωT=-1+pf0-Tp1-2p-pTpf0-Tp1-2p-T.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,z. In this manner we obtain a suitable amount for the independent parameter p to have an effective phantom-like behavior that this amount is about p=0.028. In this respect, by using the equations (28) and (29), Figures 1 and 2 are plotted. Also we have used Ωm0=0.315, H0=67.4kms-1Mpc-1, and ν=1.95 in all numerical calculations in the paper. This value p 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 (z=0) is ω0=-1.03; this amount is in favor of the recent data from Planck2018. However, we should pay attention that, in this form of f(T), the effective equation of state parameter crosses the cosmological constant (phantom divide) line, ω=-1, 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 forf(T)=T+f0(-T)p.Figure 2
Variation of effective equation of state parameter versus the redshift forf(T)=T+f0(-T)p, where the dash lines represent ω0(T)=-1.03.


## 3.2. Phantom-Like Effect withf(T)=T+ξT(1-eαT0/T)

In this modelα is an independent parameter and T0=T(z=0) is the current value of the torsion scalar. In the limit α→0, this model recovers the ΛCDM model [34]. Also, by using the modified Friedmann equation, we find(30)ξ=-1-Ωm01-1-2αeα. In this model, if α>0 the universe has a phantom phase (with ω<-1) and if α<0 it has a quintessence phase (with ω>-1) [48]. For this form of f(T) function we obtain(31)FT=ξT1-eαT0/T,(32)FT=ξαT0TeαT0/T+ξ1-eαT0/T,and(33)FTT=-α2T02ξT3eαT0/T. Once again, using (20) and (21) we acquire ρ(T) and ω(T) in the present model as follows:(34)ρT=2αξT0eαT0/T+Tξ1-eαT0/T16πG, and(35)ωT=-1+TξeαT0/T-1-2ξαT0eαT0/T-Tξ-ξeαT0/T1-αT0/T+2α2T02/T2TξeαT0/T-1-2ξαT0eαT0/Tξ-ξeαT0/T1-αT0/T+2α2T02/T2+1, 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 ρ(T) and ω(T) versus the redshift, z, for different choices of the model parameter α. Our analysis shows that the phase of expansion of the universe (according to the values of ω) depends on the sign of the parameter α. We find that α=0.07 is the acceptable value for realization of an effective phantom-like behavior in this model. By using (34) and (35), the evolutions of ρ(T) and ω(T) 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 ω(T)=-1.03 for present time. Also Figure 4 shows that the effective equation of state stays always less than -1 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 forf(T)=T+ξT(1-eαT0/T).Figure 4
Variation of effective equation of state parameter versus the redshift forf(T)=T+ξT(1-eαT0/T), where the dash lines represent ω0(T)=-1.03.


## 3.3. Phantom-Like Effect withf(T)=T+n(T-Te(βT0/T)+(-T)β)

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 mentionedf(T) 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 f(T) 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 ξ=f0≡n and p=α≡β. Here β and n are two parameters of model; only β is free parameter because n can be obtained as(36)n=-Ωm0-11-2β6H02β-2+1-1-2βeβ. Also for this combined model, we can acquire(37)FT=nT-TeβT0/T+-Tβ,(38)FT=nβT0TeβT0/T+n1-eβT0/T-nβ-Tβ-1,and(39)FTT=-nβ2T02T3eβT0/T+nββ-1-Tp-2. 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:(40)ρT=n-Tβ2β-1+T+eβT0/T2βT0-T16πG, and(41)ωT=-1+ΘΥ, where we have defined(42)Θ≡n-Tβ1-2β+eβT0/TTn-2nβT0-T1+n-Tn1-2β+eβT0/TT-2βT0-T and(43)Υ≡1+βT0/T-2β2T02/T2-1eβT0/T+1-2ββ-Tβ-11+nβT0/T-2β2T02/T2-1eβT0/T+n+nβ1-2β-Tβ-1.Finally, to investigate the possible realization of the phantom-like behavior in this combined model, by using (40) and (41), we plot ρ(T) and ω(T) versus the redshift for different values of β. 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 -1, are satisfied if β=0.2. This typical behavior of ρ(T) and ω(T) 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 ω(T)=-1 line at 0.5<zcross<1 and amount ω(T) for current time (z=0) 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 forf(T)=T+n(T-Te(βT0/T)+(-T)β).Figure 6
Variation of effective equation of state parameter versus the redshift forf(T)=T+n(T-Te(βT0/T)+(-T)β), where the dash lines represent ω0(T)=-1.03.


## 4. Conclusion

In this paper, we have investigated possible realization of an effective phantom behavior in some viablef(T) 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 -1. We have chosen three different models of f(T) 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 f(T)=T+f0(-T)p realizes an effective phantom-like behavior if p=0.028. As is shown in Figure 2, we obtained the effective equation of state parameter for present time about ω0(T)=-1.03, 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 f(T) model, which is f(T)=T+ξT(1-eαT0/T). This f(T) model realizes an effective phantom-like behavior if α=0.07. Although ω0(T) is obtained as an acceptable value that is shown in Figure 4, this f(T) 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 f(T) theory by combining the two previous models, where it only contains one model parameter β. This model realizes an effective phantom-like behavior if β=0.2. 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 ω(T) can cross the ω=-1 line at 0.5<zcross<1 and amount ω0(T) is consistent with the resent observational data. Therefore, this combined model is in agreement with the observational data.



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*Source: 4026856-2019-03-20.xml*