Interacting Holographic dark energy in chameleon tachyon cosmology

Interacting Holographic dark energy in chameleon tachyon cosmology

H. Farajollahi hosseinf@guilan.ac.ir Department of Physics, University of Guilan, Rasht, Iran    A. Ravanpak aravanpak@guilan.ac.ir Department of Physics, University of Guilan, Rasht, Iran    G. Farpour Fadakar gfadakar@guilan.ac.ir Department of Physics, University of Guilan, Rasht, Iran
July 15, 2019
Abstract

We propose in this paper an interacting holographic dark energy (IHDE) model in chameleon–tachyon cosmology by interaction between the components of the dark sectors. In the formalism, the interaction term emerges from the scalar field coupling matter lagrangian in the model rather than being inserted into the formalism as an external source for the interaction. The correspondence between the tachyon field and the holographic dark energy (HDE) densities allows to reconstruct the tachyon scalar field and its potential in a flat FRW universe. The model can show the accelerated expansion of the universe and satisfies the observational data.

Interacting holography; dark energy;
chameleon; tachyon; distance modulus

I Introduction

The universe acceleration, shown by several astronomical observations, indicates the existence of a mysterious exotic matter called dark energy (DE) Riess (Riess 1998). In the classical gravity, whereas the cosmological constant, , is the most prominent candidate of DE with the equation of state (EoS) parameter equals -1 Weinberg (Sahni 2000), there are strong evidence for a dynamical DE equation of state. However, the problem of DE, its energy density and EoS parameter is still an unsolved problem in classical gravity and may be in the context of quantum gravity we achieve a more inclusive insight to its properties Cohen (Cohen 1999). The HDE model is an attempt to apply the nature of DE within the framework of quantum gravity Hsu (Hsu 2004). The holographic principle states that the number of degrees of freedom describing the physics inside a volume (including gravity) is bounded by the area of the boundary which encloses this volume and thus relates to entropy scales with the enclosing area of the system Hooft (Susskind 1995). Since the entropy scales like the area rather than the volume, the fundamental degrees of freedom describing the system are characterized by an effective quantum field theory in a box of size with one fewer space dimensions and with planck-scale UV cut-off Setare5 (Setare 2007).

As pointed out by the author in Myung (Myung 2005), in quantum field theory, short distance cut-off is related to long distance cut-off due to the limit set by forming a black hole. In other words, if is the quantum zero-point energy density caused by a UV cut-off , the total energy of the system with size should not exceed the mass of the same size black hole, i.e. , where denotes Planck mass Liu (Zhang 2007). For the largest , holographic energy density is given by,

(1)

in which c is a free dimensionless parameter and coefficient three is for convenience Mohseni (Mohseni 2007). Assuming as the universe current size, the Hubble radius , then the DE density is close to the observational result, which we identify with the radius of the future event horizon,

(2)

where is scale factor of the universe Wang (Wang 2005). Choosing the future event horizon as the UV cut-off allows us to construct a satisfactory HDE model for the universe accelerating expansion which presents a dynamical view of the DE and is consistent with observational data Zhang (Zhang 2005).

The Interacting HDE (IHDE) models have been widely investigated in last few years Q (Gong 2008). Among all, the stability analysis of the IHDE solutions and their dynamical characteristics Setare4 (Setare 2009), IHDE due to the bulk-brane interaction Setare2 (Setare 2006) and IHDE in non-flat cosmological model Setare1 (Setare 2006) are of particular interest.

In particular, relevant works in the holographic tachyon models in both interacting and non interacting cases can be found in Bagla (Bagla 2003)Setare3 (Setare 2007)Setare5 (Setare 2007). In here, we would like to extend the previous works carried out in the IHDE models, by studying a chameleon-tachyon cosmological model. In our model the scalar field in the formalism plays two roles; as a chameleon field interacts with the matter in the universe and as a tachyon field plays the role of DE. In the previous works in IHDE models, the interacting term between IHDE and dark matter (DM) is not unique and its introduction in the formalism based on phenomenological grounds in studying a suitable coupling between quintessence scalar field and pressureless cold dark matter (CDM) to alleviate the coincidence problem Wang (Wang 2005). However, in our work the interacting term naturally appears in the model from the interaction between chameleon field and matter field in the universe in the formalism.

Ii The Model

We consider the chameleon gravity in the presence of CDM with a tachyon potential in the action given byRavanpak (Farajollahi 2011)Ravanpak2 (Farajollahi 2011),

(3)

where is Ricci scalar. Unlike the usual Einstein-Hilbert action, the matter Lagrangian is modified as , where is an analytic function of . This last term in the Lagrangian brings about the nonminimal interaction between the matter and chameleon field. The variation of action (3) with respect to the metric tensor components in a spatially flat FRW cosmology yields the following field equations,

(4)
(5)

where . In the above, we also assumed a perfect fluid filled the universe with the EoS . We can rewrite the above equations as,

(6)
(7)

where and are respectively the energy density and pressure of the tachyon. The variation of the action (3) with respect to the scalar field provides the wave equation for the scalar field as

(8)

where prime ” ” indicated differentiation with respect to and . The scalar field as a tachyon field plays the role of IHDE and by coupling with the matter field as a chameleon field plays the role of DM. Then, by their interaction, the energy densities no longer satisfy independent conservation laws, rather, they obey:

(9)
(10)

where ”ch” stands for chameleon, and is the interaction term. In , gauges the intensity of the coupling between matter and chameleon field. For , there is no interaction between DM and IHDE. The term measures the different evolution of the DM due to its interaction with the IHDE which gives rise to a different universe expansion. The remarkable point concerning the interaction term is that in comparison to the other IHDE models where the form of the interaction term is not unique and built into the formalism from the outset, in our model the interaction term naturally appears in the model directly as a function of the chameleon coupling function and and indirectly as a function of Hubble parameter and . For the decay of HDE into DM in the interaction we have to take to be positive similar to the case of in the interaction term introduced in other works Edmund (Copeland 2005).

In order to impose the holographic nature to the tachyon, one should identify the energy density of tachyon field with the energy density of the cosmological constant. From the definition of the holographic energy density, equation (1), and that of the future event horizon (2) we obtain Z (Zhang 2005)X (Zhang 2007),

(11)

where the derivative in here and from now on is with respect to , also, and . We can rewrite equation (10) as

(12)

From equations (11) and (12) we drive the dynamical EoS parameter as

(13)

We have to note, however, that although the above EoS parameter attributed to the tachyon field, the presence of the in the interaction term is directly related to the chameleon field and DM. So the situation is somewhat ambiguous due to entanglement of the DE and DM. Under these conditions, one can not easily classify the quintessence or phantom unless the interacting term is very weak according to observations. Using equations (12) and (13) and the definition of we find

(14)

Also, by replacing and into the acceleration equation (5), one obtains,

(15)

From equations (14) and (15), we drive the evolution equation for in terms of the redshift as,

(16)

which controls the dynamics of the IHDE model. From equation (15), the evolution of the Hubble parameter with respect to the redshift can be expressed as

(17)

Using equation (6), and , we derive the interacting holographic tachyon potential,

(18)

where is the critical energy density of the universe at the present epoch. In addition, using the relation , the evolution of the interacting holographic tachyon scalar field with respect to the redshift z becomes,

(19)

where the sign is arbitrary and can be changed by a redefinition of the field, . Then, by fixing the field amplitude at the present era to be zero, one may obtain the dynamic of the holographic tachyon field. It is difficult to solve equations (16)-(19) analytically, however, the evolutionary form of the interacting holographic tachyon field and can be easily obtained by integrating it numerically from to a given value . In addition, from the constructed holographic tachyon model, the evolution of with respect to can be determined.

In the following numerical computation, we assume that the function behaves exponentially as . Since is present in the interaction term , the parameters that directly determine the dynamics of the interaction are and together with and . Note that or leads to the absence of the interaction.

In Fig. 1 and 2, by solving the equations (16)-(19), the reconstructed scalar field and are shown. The curves are plotted for different values of , , and with the fractional matter density selected to be . From Fig. 2, the reconstructed tachyon potentials are more steep in the early epoch () and tending to be flat in near future when the scalar field is negative. Therefore, the tachyon scalar field rolls down the potential more slowly with the kinetic energy gradually decreasing in near future where from Fig. 3a the tachyon EoS parameter become tangent to -1 when . This scenario is similar to the holographic quintessence scenario L (Granda 2009). Note that, from Fig.1, the tachyon scalar field increases with , becomes finite at high redshift and decreases as the universe expands. Note also that, due to smallness of interaction term, the behavior of the holographic scalar field is similar in the presence and absence of the interaction term which is compatible with the observational data Setare3 (Setare 2007).

Figure 1: The behavior of the scalar field with respect to , for different parameters , , and where is in unit of . (a) , (b) , (c)
Figure 2: The behavior of the potential for the interacting holographic tachyon model with respect to , for different parameters , , and where is in unit of and in . (a) , (b) , (c)

In addition, the dynamics of the ratios of the energy densities of the HDE, , and DM, , to the critical energy density in the universe are shown in Fig.3b. The graph shows that the impact of the interaction between IHDE and DM increases at a faster rate compared to the non-interacting case. It also shows that in the presence of interaction the domination of HDE occurs later in .

Figure 3: Variation of and with respect to redshift for the holographic tachyon model with and without interaction. We put and

From the above equations one can easily obtain the total EoS and deceleration parameters for the model as,

(20)
(21)

In Fig. 4, the deceleration parameter for different parameters , and are shown. Figs. 4a) and 4c), for a fixed , show the effect of interaction term on the acceleration of the universe. From these graphs, since in the interaction the IHDE decays into DM, the cosmic acceleration starts later with interaction compare to the case without interaction since IHDE dominates later. Also for larger interaction, since more IHDE decays into DM, the acceleration starts later.

Figure 4: The behavior of the deceleration parameter with respect to , for different parameters , , and . (a) , (b) , (c)

Noting that in the constructed holographic model, equations (16)-(19) satisfy the condition . On the other hand, the observational data constrains the value. However, the latest observational data, including the SNe Ia, the CMB shift parameter given by the WMAP observations, and the BAO measurements from SDSS, show the possibilities of both and , and their likelihood are almost equal within error rangeSetare3 (Setare 2007)Liu (Zhang 2007).

Iii Cosmological Test

Luminosity distance quantity, , determines DE density from observations. In our model with the obtained from numerical calculation, we have

(22)

The difference between the absolute and apparent luminosity of a distance object called distance modulus, , and is given by . In Fig. 5, we compare our model for the distance modulus with the observational data. Here, we have used recent observational data, including Sne Ia which consists of 557 data points belonging to the Union sampleAman (Amanullah 2010).

Figure 5: Plot of the distance modulus, , with respect to the redshift for two different values of , in comparison with the observational data. We put and

The graph shows that for the distance modulus obtained from numerical calculation for the model better fits the observational data.

Iv Summary and Remarks

In this work we have proposed a holographic model of tachyon-chameleon cosmology by taking into account the holographic principle of quantum gravity; by implementing a combination of holographic DE model and interacting tachyon chameleon fields. In Setare3 (Setare 2007) the holographic dark energy is described by the tachyon field in a certain way. Then a correspondence between the HDE and tachyon model of dark energy has been established in two different cases, flat and non-flat FRW universes. The author has shown that the value of is a key point to the feature of the HDE and the ultimate fate of the universe as well.

In holographic models, one considers that the scalar field models of DE are effective theories of an underlying theory of DE. In particular, the tachyon scalar field carries some holographic feature that with is capable of realizing the holographic evolution of the universe. In our model, by connection between the tachyon and the holographic DE, the potential of the holographic tachyon has been constructed. Although the effect of the interaction term is very small, the possibility of a small, but calculable, interaction in the dark sector remains open, and future investigations, with more realistic models and more observational data are necessary to solve this problem Sandro (Sandro 2010). The scalar field in our formalism plays two roles; as a chameleon field interacts with the matter in the universe and as a tachyon field plays the role of DE. In the more familiar models, the interacting term between IHDE and DM is introduced in the formalism based on phenomenological grounds in studying a suitable coupling between quintessence scalar field and pressureless CDM to alleviate the coincidence problem Wang (Wang 2005). In our work, different from other approaches, the interacting term naturally appears in the model from the interaction between chameleon and matter fields in the universe. The interaction terms is similar to the proposed ones introduced in the IHDE models. A comparison of the model with recent observational data shows that for the parameter greater than one, the model for distance modulus better fits the observational data.

In Setare2 (Setare 2006) and Setare1 (Setare 2006) the author considered measured from the sphere of the horizon, as system’s IR cut-off and obtained the equation of state for the interacting holographic energy density in the non-flat universe. Further, in Setare2 (Setare 2006) the effects of the interaction between a brane universe and the bulk and in Setare1 (Setare 2006), between holographic energy density and CDM are studied. In our paper, the tachyon field in connection with IHDE shows a quintessence like equation of state parameter in the past that become tangent to the phantom divide line in future. The deceleration parameter in the model shows a transition from deceleration to acceleration at about in the past for different model parameters compatible with recent observational data.

References

  • (1) Riess, A. G., et al. 1998, J. Astron. 116, 1009
  • (2) Sahni, V. Starobinsky, A. A. 2000, Int. J. Mod. Phys. D 9, 373
  • (3) Cohen, A.G., Kaplan D.B. & Nelson, A. E.1999 ,prl 82, 4971
  • (4) Hsu,S. D. H. 2004, Phys. Lett. B 594, 13
  • (5) Susskind, L. 1995, J. Math. Phys, 36,6377
  • (6) Farajollahi, H., Ravanpak, A. & Fadakar, G. F. 2011, Mod. Phys. Lett. A Vol. 26, No. 15 1125-1135
  • (7) Farajollahi, H., Salehi, A., Tayebi, F. & Ravanpak, A. 2011, jcap 05, 017
  • (8) Myung,Y. S.2005, Phys. Lett. B 610,18
  • (9) Zhang, J., Zhang, X. & Liu, H.2007, Phys. Lett. B 651, 84
  • (10) Mohseni Sadjadi, H. 2007, jcap 0702, 026
  • (11) Wang, B., Gong, Y. g. & Abdalla, E.,2005, Phys. Lett. B 624, 141
  • (12) Zhang, X., Wu,F.Q. 2005 prd 72, 043524
  • (13) Wu, Q., Gong, Y., Wang, A. & Alcaniz,J.S. 2008, Phys. Lett. B 659, 34
  • (14) Bagla, J. S., Jassal, H. K. & Padmanabhan,T.,2003, prd 67, 063504
  • (15) Copeland,E. J., Garousi,M. R., Sami,M. & Tsujikawa, S.,2005, prd 71, 043003
  • (16) Zhang,X.,2005, Int. J. Mod. Phys. D 14, 1597
  • (17) Zhang, X.2007, Phys.Lett. B 648, 1
  • (18) Granda, L. N. 2009, Int. J. Mod. Phys.D 1749
  • (19) Sandro Micheletti, M. R. 2010 jcap, 1005, 009
  • (20) Setare, M.R. 2006 Phys. Lett. B 642:421-425
  • (21) Setare, M.R. 2006 Phys. Lett. B 642:1-4
  • (22) Setare, M.R. 2007 Phys. Lett. B 653:116-121
  • (23) Setare, M. R. 2007 jcap 0701, 023
  • (24) Setare, M.R., Vagenas Elias C. 2009 Int. J. Mod. Phys.D 18:147-157
  • (25) Amanullah, R., et al. 2010 Astrophys. J. 716:712-738
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