Modified Holographic Dark Energy in Non-flat Kaluza-Klein Universe with Varying G

Modified Holographic Dark Energy in Non-flat KaluzaKlein Universe with Varying

M. Sharif and Abdul Jawad
Department of Mathematics, University of the Punjab,
Quaid-e-Azam Campus, Lahore-54590, Pakistan.
msharif.math@pu.edu.pkjawadab181@yahoo.com
Abstract

The purpose of this paper is to discuss the evolution of modified holographic dark energy with variable in non-flat KaluzaKlein universe. We consider the non-interacting and interacting scenarios of the modified holographic dark energy with dark matter and obtain the equation of state parameter through logarithmic approach. It turns out that the universe remains in different dark energy eras for both cases. Further, we study the validity of the generalized second law of thermodynamics in this scenario. We also justify that the statefinder parameters satisfy the limit of CDM model.

Keywords: KaluzaKlein cosmology; Modified holographic dark energy; Dark matter; Generalized second law of thermodynamics.
PACS: 04.50.Cd; 95.36.+d; 95.35.+x; 98.80.-k

1 Introduction

The discovery of the accelerating expansion of the universe is a milestone for cosmology which has deep implications for the composition of the universe, structure formation and its fate. The expansion of the universe shows that it is not slowing down under normal gravity but accelerating due to an unknown component termed as dark energy (DE), having a strong negative pressure [1]. There are many pieces of evidence for the existence of this component of the universe other than the baryonic and non-baryonic dark matter (DM) [2] but it has no clear clue about its identity.

The most convenient explanation for this expansion is the vacuum energy that generates sufficient force to push matter apart described by cosmological constant [2]. However, there are two alternative ways used extensively in order to explain this behavior. The first approach is the work on different DE models such as quintessence [3], K-essence [4], phantom [5], quintom [6], tachyon [7], family of Chaplygin gas [8], holographic [9, 10] and new agegraphic DE [11]. Among all these models, holographic DE models are widely used. They provide the link of the DE density to the cosmic horizon [12] and has been tested through various astronomical observations [13].

The idea of holographic DE model (HDE) can be extracted from the holographic principle, which states that the number of degrees of freedom of a physical system should scale with its bounding area rather than its volume [14]. Cohen et al. [15] proposed a relation of ultraviolet (UV) and infrared (IR) cutoffs due to the limit set by forming a black hole in quantum field theory. In their point of view, the total energy of the system having size is bounded by the mass of black hole of the same size. Mathematically, it can be written as , where represents the vacuum energy density and is the reduced Planck mass. Thus one can deduce holographic DE [9]

here constant is used for convenience and .

The variation of Newton gravitational constant with cosmic time has been considered for discussing the evolution of DE models. This was also used for solving the longstanding problems such as the DM problem, the controversies of Hubble parameter value and the cosmic coincidence problem (references therein [16]). Additionally, a lot of debate is available in literature for the choice of IR cutoff: whether it is a Hubble horizon, or particle horizon, or future event horizon for flat FRW universe. It was pointed out by Li [10] that the future event horizon is the appropriate choice for IR cutoff which favors the current observations.

The modified and multidimensional theories of gravity (including f(), f(), f(,) [17], f() [18], BransDicke [19], HoravaLifshitz [20], Kaluza
Klein (KK) [21]) is the second approach in which a phenomenon to modify the gravitational sector or increment of dimension takes place. In case of higher dimensional theories, KK theory has attracted many people recently to discuss the DE puzzle. It exists in two versions: compact (fifth dimension is length like and it should be very small) and non-compact forms (fifth dimension is mass like) [22]. In addition, on the basis of the dimensional mass of the Schwarzschild black hole [23], Gong and Li [24] derived the HDE in extra dimensions (called modified holographic dark energy (MHDE)).

A marvellous work is available which investigates the non-interacting [10, 25, 26] and interacting [27] possibilities of HDE with DM in flat and non-flat FRW universes. The thermodynamical interpretation of HDE model with different IR cutoff was also investigated by many people [28, 29] for non-flat FRW universe. The proposal of a statefinder was given by Sahni el al. [30] for characterizing and differentiating various DE models. Alam et al. [31] proved that these parameters are a useful tool for describing the properties of DE models. Some people [32]-[35] have obtained interesting results about HDE with the help of these parameters. Also, MHDE has been considered to discuss the evolution of the universe [24, 36]. Recently Sharif et al. [37, 38] have explored the evolution of interacting MHDE with Hubble horizon and event horizon as an IR cutoff in a flat KK universe and also examined the validity of generalized second law of thermodynamics (GSLT).

This paper is devoted to study the evolution of non-interacting and interacting MHDE in a non-flat KK universe. The sequence of paper is as follows: we discuss the evolution of non-interacting and interacting MHDE in non-flat universe in the next section. In section 3, the generalized second law of thermodynamics is explored. Section 4 contains the discussion of statefinder. We summarize our results in section 5.

2 Modified Holographic Dark Energy and
Non-flat KaluzaKlein Universe

In this section, we evaluate equation of state (EoS) parameter for the non-interacting and interacting MHDE with DM in a compact non-flat KK universe [39] whose line element is

(1)

where a(t) is the cosmic scale factor responsible for the expansion of the universe and is the spatial curvature which corresponds to open, flat and closed universe, respectively. The Einstein field equation in dimensions are

(2)

where and represent the Ricci tensor, the metric tensor, the Ricci scalar, the energy-momentum tensor and the coupling constant, respectively. Also, we assume that the KK universe is filled with perfect fluid whose energy-momentum tensor is given by

(3)

where is the pressure due to DE, is the DE plus DM (dust like) energy densities and is the five velocity satisfying the relation , respectively. Using Eqs.(2) and (3), we get the following Einstein field equations for non-flat KK universe:

(4)
(5)

Here is the Hubble parameter and dot is the differentiation with respect to time. Equation (4) can be written in terms of fractional energy densities as

(6)

where

(7)

The MHDE in dimensions is given as [24]

where and indicate the area of unit -sphere and volume of the extra-dimensional space, respectively. In case of the KK cosmology, it becomes

(8)

Here is defined for non-flat KK universe as [25]

(9)

where is obtained through the relation

Further, its integration gives

is the the future event horizon which is defined as

The time derivative of yields

(10)

with

Using Eqs.(8) and (10), we obtain the evolution of energy density

(11)

where and prime represents derivative with respect to . By differentiating fractional energy densities , and using Eq.(10), it follows that

(12)

In the following, we investigate EoS parameter for non-interacting and interacting cases.

2.1 Non-Interacting Case

The equation of continuity for the KK universe is

We consider the universe filled with DE and DM which splits it into two equations for DM and DE, respectively, as

(13)
(14)

In order to eliminate the term including in Eq.(12), we use Eqs.(4), (8) and (13):

Inserting this value in Eq.(12), it follows that

Now we want to extract EoS parameter in terms of redshift parameter . Integration of the conservation equation for DE gives

We follow the procedure of Li [10] and use Taylor expansion of the DE density around the present time as

where is the present value of the DE density. The EoS parameter, up to second order expansion, becomes

(17)

here we have assumed the small redshift approximation, i.e., , where

(18)

From (7) and (13), one can get

(19)

Making use of Eqs.(LABEL:14), (18) and (19), it follows that

(20)
(21)
Figure 1: Plot of versus for non-interacting case.

where () denotes the present time value of the parameters.

Finally, we obtain by inserting the above equations in (17). In the evolution of , the MHDE parameter plays a crucial role and hence we plot against as shown in Figure (1). Here we consider the present values of fractional energy densities , , [40] and [16]. Plots in turquoise, blue, pink and green curves correspond to values of redshift parameter respectively. We observe that for , the EoS parameter attains different phases of the universe such as phantom (), vacuum DE (), quintessence () and then phantom for . However, for , the EoS achieves its maximum value , respectively, and remains in the phantom region except .

2.2 Interacting Case

Here we evaluate EoS parameter in the interacting phenomenon of MHDE with DM by using the same procedure as above. In this case, the equation of continuity may be converted into two non-conserving equations for DM and MHDE, respectively, i.e.,

(22)
(23)

where denotes the interaction term which can be taken as [27]

The parameter is a coupling constant and the selection of its square leads to the condition of decay from DE to DM. We can find and by using the above procedure as follows:

(24)
(25)
Figure 2: Plot of versus for interacting case.

Inserting these values in Eq.(17), we obtain EoS parameter. In this case, evolves two constant parameters and (interacting parameter). Figure (2) shows the plot of against by setting and the remaining parameters are the same as in the non-interacting case. Notice that the maximum values of EoS parameter corresponding to the redshift parameter becomes smaller than that of the non-interacting case.

3 Generalized Second Law of Thermodynamics

Now we investigate the validity of GSLT for non-interacting and interacting MHDE with varying G in the non-flat KK universe. According to this law, the sum of entropy of matter inside and at the event horizon remains always positive with the passage of time [41]. Thermodynamics of black hole plays the role of pillar for thermodynamical interpretation of the universe. Bekenstein [42] suggested that, in view of the proportionality relation between entropy of black hole horizon and horizon area, the sum of black hole entropy and the background entropy must be an increasing quantity with time. The first law of thermodynamics gives

(26)

where and represent temperature, entropy, internal energy and pressure of the system, respectively. Splitting this law for DE, DM and differentiating with respect to time, we obtain

(27)

The volume, temperature and entropy of horizon in KK universe become [43]

(28)

Also, we require the following thermodynamical quantities:

(29)

Equation (6) can be re-written as

(30)

In view of the above equations, we have

(31)

where is the sum of three entropies. When we substitute the present values of , (with ) and in the above expression, it remains non-negative for both interacting and non-interacting cases of MHDE i.e., .

4 The Statefinder Diagnostic

Here we explore the behavior of statefinder parameters in the above mentioned scenario. These parameters have geometrical diagnostic due to their total dependence on expansion factor. These are defined for a non-flat KK universe as [44]

(32)

where and is the deceleration parameter defined as

(33)

The statefinder parameters are dimensionless and exhibit expansion of the universe through higher derivatives of the scale factor. These are a natural companion to the deceleration and Hubble parameters. The pair defines the well-known CDM model at the fixed point . Moreover, can be expressed in terms of the Hubble parameter as

(34)

With the help of Eqs.(33) and (34), one can write

(35)

In the non-interacting case, the time derivative of the deceleration parameter becomes

Inserting this in Eq.(35), we obtain

(36)
(37)

For the interacting case, we differentiate Eq.(5), using (11) and (2.1), and it follows that

Figure 3: Plots of versus for (a) non-interacting and (b) interacting cases.

Consequently, the corresponding statefinder takes the form

(38)
(39)

We can easily find a single relation of in terms of and draw plane as shown in Figure (3) for () non-interacting and () interacting MHDE. Plots in pink, blue, turquoise and green colors are drawn at different physically acceptable values of (as already discussed in [38]), respectively, for non-interacting as well as interacting cases. Also, we fix and recover the CDM model in both cases.

5 Concluding Remarks

We have investigated the behavior of EoS parameter, GSLT and statefinder for the MHDE (non-interacting and interacting with DM) with variable correction in non-flat KK universe enclosed by future event horizon. Actually, the MHDE exhibits the dynamical nature of the vacuum DE through its parameter . We have evaluated the EoS parameter with respect to for different ranges of . It is found that the interacting and non-interacting MHDE behave like a quintom model for a comparatively smaller value of the redshift parameter, i.e., with the assumptions of the present values of the other parameters. For other values of , it evolutes the universe in phantom DE era in view of increasing . Our results about evolution of MHDE with varying shows compatibility with the present observations for flat, non-flat FRW [16, 26] and flat KK universes [38] enclosed by future event horizon that it can cross the phantom divide.

Secondly, we have explored that GSLT is satisfied with for the universe describing phantom evolution. Moreover, we have obtained the evolution of non-interacting and interacting MHDE in the statefinder plane for different best fitted values of (for interacting case) and . The trajectories of - plane have been achieved with respect to different model parameters which is started from right to left. Notice that the parameters and show decreasing and increasing behavior, respectively, with the phantom evolution of the KK universe.

References

  • [1] Riess, A.G. et al.: Astron. J. 116(1998)1009; Perlmutter, S. et al.: Astrophys. J. 517(1999)565.
  • [2] Peebles, P.J.E.: Rev. Mod. Phys. 75(2003)559.
  • [3] Ratra, B and Peebles, P.J.E.: Phys. Rev. D37(1988)3406.
  • [4] Armendariz-Picon, C., Damour, T and Mukhanov, V.: Phys. Lett. B458(1999)209; Chiba, T., Okabe, T. and Yamaguchi, M.: Phys. Rev. D62(2000)023511.
  • [5] Caldwell, R.R.: Phys. Lett. B545(2002)23; Carroll, S.M., Hoffman, M. and Trodden, M.: Phys. Rev. D68(2003)023509.
  • [6] Feng, B., Wang X.L. and Zhang, X.M.: Phys. Lett. B607(2005)35.
  • [7] Padmanabhan, T.: Phys. Rev. D66(2002)021301; Bagla, J.S., Jassal, H.K. and Padmanabhan, T.: Phys. Rev. D67(2003)063504.
  • [8] Kamenshchik, A.Y., Moschella, U. and Pasquier, V.: Phys. Lett. B511(2001)265; Bento, M.C., Bertolami, O. and Sen, A.A.: Phys. Rev. D 66(2002)043507; Zhang, X., Wu, F.Q. and Zhang, J.: JCAP 01(2006)003.
  • [9] Hsu, S.D.H.: Phys. Lett. B594(2004)13.
  • [10] Li, M.: Phys. Lett. B603(2004)1.
  • [11] Cai, R.G.: Phys. Lett. B657(2007)228.
  • [12] Ng, Y.J.: Phys. Rev. Lett. 86(2001)2946; Arzano, M., Kephart, T.W. and Ng, Y.J.: Phys. Lett. B649(2007)243.
  • [13] Zhang, X. and Wu, F.Q.: Phys. Rev. D72(2005)043524.
  • [14] Susskind, L.: J. Math. Phys. 36(1995)6377.
  • [15] Cohen, A., Kaplan, D. and Nelson, A.: Phys. Rev. Lett. 82(1999)4971.
  • [16] Jamil, M., Saridakis, E.N., and Setare, M.R.: Phys. Lett. B679(2009)172.
  • [17] Nojiri, S. and Odintsov, S.D.: Int. J. Geom. Meth. Mod. Phys. 4(2007)115.
  • [18] Linder, E.V.: Phys . Rev. D81(2010)127301.
  • [19] Brans, C.H. and Dicke, R.H.: Phys. Rev. 124(1961)925.
  • [20] Dutta, S and Saridakis, E.N.: JCAP 01(2010)013.
  • [21] Kaluza, T.: Zum Unitatsproblem der Physik Sitz. Press. Akad. Wiss. Phys. Math. k1 (1921)966; Klein, O.: Zeits. Phys. 37(1926)895.
  • [22] Wesson, P.S.: Gen. Relativ. Gravit. 16(1984)193; Spacetime-Matter Theory (World Scientific, 1999); Bellini, M.: Nucl. Phys. B660(2003)389.
  • [23] Myers, R.C.: Phys. Rev. D35(1987)455.
  • [24] Gong, Y. and Li, T.: Phys. Lett. B683(2010)241.
  • [25] Huang, Q.G. and Li, M.: JCAP 04(2004)013.
  • [26] Lu, J. et al.: JCAP 03(2010)031.
  • [27] Sheykhi, A.: Phys. Rev. D84(2011)107302; Karami, K., Ghaffari, S. and Soltanzadeh, M.M.: Class. Quantum Grav. 27(2010)205021.
  • [28] Setare, M.R.: JCAP 01(2007)023; Sheykhi, A.: Class. Quantum Grav. 27(2010)025007.
  • [29] Mazumder, M. and Chakraborty, S.: Gen. Relativ. Gravit. 42(2010)813.
  • [30] Sahni, V. et al.: JETP Lett. 77(2003)201.
  • [31] Alam, U. et al.: Mon. Not. R. Astron. Soc. 344(2003)1057.
  • [32] Feng, C.: Phys. Lett. B670(2008)231.
  • [33] Setare, M.R., Zhang, J. and Zhang, X.: JCAP 03(2007)007; Setare, M.R. and Jamil, M.: Gen. Relativ. Gravit. 43(2011)293.
  • [34] Malekjani, M., Khodam-Mohammadi, A. and Nazari-pooya, N: Astrophys. Space Sci. 332(2011)515.
  • [35] Chakraborty, S. et al.: Int. J. Theor. Phys. (2012, to appear), arXiv:1111.3853.
  • [36] Liu, D.J., Wang, H. and Yang, B.: Phys. Lett. B694(2010)6.
  • [37] Sharif, M. and Khanum, F.: Gen. Relativ. Gravit. 43(2011)2885.
  • [38] Sharif, M. and Jawad, A.: Astrophys. Space Sci. 337(2012)789.
  • [39] Ozel, C., Kayhan, H. and Khadekar, G.S.: Ad. Studies. Theor. Phys. 4(2010)117.
  • [40] Paul, B.C., Debnath, P. S. and Ghose, S.: Phys. Rev. D79(2009)083534.
  • [41] Izquierdo, G. and Pavn, D.: Phys. Lett. B633(2006)420.
  • [42] Bekenstein, J.D.: Phys. Rev. D7(1973)2333.
  • [43] Cai, R.G. and Kim, S.P.: JHEP 0502(2005)050.
  • [44] Evans, A.K.D. et al.: Astron. Astrophys. 430(2005)399.
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
254199
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description