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Advances in High Energy Physics
Volume 2013 (2013), Article ID 790967, 10 pages
Research Article

Analysis of Theory Corresponding to NADE and NHDE

Department of Mathematics, University of the Punjab, Quaid-e-Azam Campus, Lahore 54590, Pakistan

Received 31 January 2013; Revised 1 April 2013; Accepted 29 April 2013

Academic Editor: Piero Nicolini

Copyright © 2013 M. Sharif and M. Zubair. 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.


We develop the connection of theory with new agegraphic and holographic dark energy models. The function is reconstructed regarding the theory as an effective description for these dark energy models. We show the future evolution of and conclude that these functions represent distinct pictures of cosmological eras. The cosmological parameters such as equation of state parameter, deceleration parameter, statefinder diagnostic, and analysis are investigated which assure the evolutionary paradigm of .

1. Introduction

Expanding paradigm of the universe has been affirmed by the contemporary observational data [15]. The prime source behind this dramatic change in the evolution of the universe is said to be dark energy (DE). Dark energy is a strange type of gravitationally repulsive energy component, spreading over 72% of the contents in the universe. The nature of DE is still a question mark, and various representations have been proposed in general theory of relativity to understand it. Holographic dark energy (HDE) appeared as one of the most eminent candidates to address the issue of cosmic acceleration. The density of the HDE has been proposed by incorporating the mathematical form of the holographic principle as [6, 7] where is a constant, is the reduced Planck mass, and is the infrared (IR) cutoff. Though Hubble horizon is the natural possibility for , it does not imply the cosmic acceleration [8]. Li [7] suggested that the future event horizon is the most appropriate choice for IR cutoff, which seems to be consistent with recent measurements.

The modification of the IR cutoff in HDE has been reported in different scenarios, such as introducing new time scale and considering as a function of the Ricci scalar in both original and generalized forms. Wei and Cai [9] suggested a new model of agegraphic DE by introducing conformal time as the time scale for the FRW universe and is known as new agegraphic DE (NADE). Wu et al. [10] discussed the evolution of the new agegraphic quintessence DE models in phase plane both with and without interaction. The NADE model has been formulated in the context of alternative theories, such as Brans-Dicke theory [11] and Hoava-Lifshitz gravity [12]. Granda and Oliveros [13, 14] proposed a new IR cutoff for HDE in terms of and and discussed the correspondence of new HDE (NHDE) with models of scalar fields. This work has been extended for interacting case in nonflat universe [15].

The modification of the Einstein-Hilbert action is another promising approach to explain the fact of cosmic acceleration. In this regard, there are various theories of gravity, such as [1619], , where is the trace of the energy-momentum tensor [2026], Gauss-Bonnet gravity [27, 28], and so forth. The action of theory with matter Lagrangian is defined as In the literature [2934], people have discussed the cosmological reconstruction of theory according to the class of HDE models. Capozziello et al. [29] developed an effective numerical scheme for reconstructing from Hubble parameter of a given DE model and applied this scheme to the quintessence DE model and Chaplygin gas.

Following [29], Wu and Zhu [30] reconstructed according to HDE and explored the future evolution for different values of the parameter . Feng [31] analyzed the effect of parameter on reconstructed corresponding to Ricci DE. The explicit functions of in FRW universe can also be obtained from the reconstruction procedure according to the given DE model. Setare [32, 33] obtained functions corresponding to HDE and NADE by assuming an ansatz for the scale factor. In [34], reconstruction has been executed for both ordinary and entropy corrected models of holographic and NADE. In a recent work [25], we have reconstructed models according to holographic and NADE and found that the said models can represent the quintessence/phantom regimes of the universe.

Here, we regard the NADE and NHDE as promising models and apply the numerical scheme for reconstructing without introducing any additional DE factor. The future evolution of is presented for different values of the essential parameters. We assure the evolution of by analyzing the corresponding behavior of cosmographic parameters in particular DE models. The paper has the following format: in Section 2, we reconstruct the theory according to NADE and discuss the future evolution. Section 3 provides the evolution of corresponding to NHDE. In Section 4, we summarize our findings.

2. Reconstruction from NADE

We consider the NADE density of the form [9] where the factor is inserted to parameterize some uncertainties, namely, the specific forms of cosmic quantum fields, the role of spacetime curvature, and so forth. And is the conformal time in FRW background

For the flat FRW geometry comprising of matter component and NADE, the Friedmann equation is given by where from the energy conservation equation of matter. By defining the fractional matter and DE densities with , the Hubble parameter is obtained as

Differentiating with respect to and making use of DE conservation equation, the equation of state (EoS) parameter in NADE is obtained as

Using (3) and (4) with the relation , we obtain where prime denotes derivative with respect to . The initial condition on can be set from (5) as

One can determine using (8) and (9), and hence, the evolution of the universe in NADE can be executed.

The field equations of theory can be found by varying action (2) with respect to the metric where originates from the curvature contribution to the effective energy-momentum tensor; the subscript denotes derivative with respect to the scalar curvature and . is the standard matter energy-momentum tensor. For the flat FRW geometry, the respective field equations together with the conservation equation are given by where and . In this discussion, we consider the pressureless matter without any curvature-matter interaction. Equation (12) can be combined to single equation Employing the relation , we replace by , and hence, (13) can be translated into 3rd-order differential equation of as where are functions of and its derivatives given by .

We aim to solve this equation to obtain using the Hubble parameter . For this purpose, we set the boundary conditions of the form [29]

If the function is known, then the coefficients and hence the function can be evaluated corresponding to the given DE model. In case of NADE, we do not have explicit form of whereas and its derivatives can be represented in terms of . Therefore, after lengthy calculations, the coefficients are interpreted in the form of and . We solve numerically the system of (8) and (14) together with the conditions (9) and (15).

In [35], the constraint on parameter is developed from the cosmological data for a flat universe consisting of DE and matter component, and the best fit value is found to be . For the nonflat universe, Zhang et al. [36] found that the most appropriate measure of from the WMAP 7-year observations is . In this study, we set and . For this choice of parameters, the function is plotted against as shown in Figure 1. It is clear that functions appear distinct if (or ) is large, while these functions seem to coincide for small . The evolution of shown in Figure 1 is quite similar to that for HDE [30]. We also plot these functions on plane as shown in Figure 2, where and . Our results are consistent with that in [29], and the parameter appears as fundamental element in identifying the nature of NADE.

Figure 1: Reconstructed for NADE with .
Figure 2: Reconstructed for NADE in plane with .

To explore the effect of further, let us see the future evolution of . Figure 3 shows that future variation of is alike for different values of and almost favors the cosmological constant. In Figures 4 and 5, we present the future evolution of for . For , the curve seems to be similar to that for in HDE, but in the late stage of the universe, there would be a sudden change. The evolution of is similar for other values of which is shown in Figure 5. These plots indicate distinct characteristics for the NADE.

Figure 3: Future evolution of in NADE with .
Figure 4: Future evolution of for with .
Figure 5: Future evolution of for different values of with .

We extend our discussion and explore the evolution of NADE for the cosmographic parameters such as EoS parameter, deceleration parameter, statefinder diagnostic, and analysis. It is clear from (7) that NADE does not permit the crossing of phantom divide line , also if and , then in future evolution of NADE. Figure 6(a) shows that for our choice of parameter , the EoS parameter of NADE favors the quintessence era, and in the late time, it mimics the cosmological constant regime. We also show the evolution of in plane for different values of in NADE. Figure 6(b) depicts that the plane represents the CDM model ) when (or ). The present values of and are denoted by dots on each curve. For , the present values of () are given by , and , respectively.

Figure 6: Evolution trajectories in NADE for (a) versus and (b) and in plane with .

Sahni et al. [37, 38] defined the statefinder diagnostic parameters of the form

Introducing the EoS parameter and dimensionless density of DE, (16) is transformed as

The deceleration parameter in terms of and is given by

The variation of deceleration parameter with for the NADE without interaction is shown in Figure 7(a). The transition of the universe from decelerating epoch to the accelerated era can be seen, and it will end up with representing the de Sitter model. The sign flip of depends on the selection of ; the era of cosmic acceleration starts earlier for small values of as compared to larger values.

Figure 7: Evolution trajectories in NADE for (a) versus and (b) the statefinder diagnostic in plane with .

The plots of statefinder parameters in the plane for are shown in Figure 7(b). The dots in the diagram correspond to present day values of statefinder parameters , which are denoted as (red), (black), (gray), and (blue). The evolution trajectories of the statefinder diagnostic are represented for the future evolution, and these will end up to star symbol , the CDM model. We also plot the statefinder diagnostic in plane for our selection of parameter together with the flat CDM model. It can be seen from Figure 8 that evolution trajectories for NADE in plane commence from the fix point , which represents the standard cold dark matter regime (SCDM). These curves end at , the de Sitter model in future evolution of the universe. The past and future eras of the universe and present day values of are represented by stars and dots, respectively.

Figure 8: The statefinder plot for NADE in plane. The green line represents the CDM with .

3. Reconstruction from NHDE

The energy density of HDE with Granda-Oliveros cutoff is given by [13, 14] where and are positive constants. Using this value of , (5) can be written in the form where , is the present day value of Hubble parameter and is the constant of integration which can be obtained using the condition as

Following [13, 14], the NHDE density is expressed as

The pressure of NHDE can be obtained using this value of in the conservation equation of DE

Manipulating (22) and (23), the EoS parameter of NHDE turns out to be

Proceeding in a similar fashion as in the case of NADE, we obtain where are functions of and its derivatives, see the appendix. For the HDE with Granda-Oliveros cutoff, the expression for is directly useable in numerical computations. If we substitute (20) and constraint (21) in differential equation (25), then the resulting equation can be solved numerically under the boundary conditions (15).

In [13, 14], the best fit values of parameters and are suggested as and to keep NHDE consistent with the theory of big-bang nucleosynthesis. Wang and Xu [39] developed the best fit values of parameters in both flat and nonflat NHDE models from the current observational data. They found the best fit parameters for the flat model as and . In this study, we select the parameters , , and . The plot of the function versus for NHDE is shown in Figure 9(a). It shows that reconstructed for NHDE is the same for different values of parameters . We also plot these results on plane as shown in Figure 9(b). To be more definite about the behavior of , we draw plot on plane presented in Figure 10. This shows that different values of parameters do not affect the shapes of curves unless , and aftermath these curves would depict different picture.

Figure 9: Reconstructed in (a) plane and (b) plane for NHDE with .
Figure 10: Reconstructed for NHDE in plane with , where .

In order to explore the distinctive effect of parameters , we get insight of future evolution. First, we investigate the future evolution of versus red shift which is shown in Figure 11. For , would take infinitely large values in future which indicate the phantom era with dominating over the matter part, leading to the big rip singularity. When , there is a slight variation in and diagram assures the DE model with , the cosmological constant. The difference in the selected parameters can be seen more effectively in the future evolution of reconstructed according to the NHDE as shown in Figures 12, 13, and 14. For and in Figure 12, the curve shows that initially decreases before reaching the present epoch , which changes its direction and it would increase leading to the phantom DE. In this scenario, keeps growing, whereas initially decreases and then attains positive value approaching to . In fact, in phantom DE models, the point of reversion is a common characteristic because the DE components succeed in their competition with matter contents of the universe. For and , we have almost identical picture as in Figure 12, but here the growing rate in is comparatively large. For and , we have a linear dependence of on leading to constant which is in accordance to the de Sitter model, where .

Figure 11: Future evolution of in NHDE with .
Figure 12: Future evolution of for with . The dot denotes the present day and is the point of reversion for DE dominated model.
Figure 13: Future evolution of for with . The dot denotes the present day and is the point of reversion for DE dominated model.
Figure 14: Future evolution of for with . The dot denotes the present day and is the point of reversion for DE dominated model.

Now, we discuss the evolution of the NHDE for the selected parameters and interpret the behavior of EoS parameter, deceleration parameter, and statefinder diagnostic. The plot of EoS parameter for future evolution in NHDE is shown in Figure 15. It shows that the NHDE represents the de Sitter phase of the universe for . For , the EoS parameter intersects the phantom divide line () and behaves as quintom model of DE [40]. In this perspective, ends up with phantom era which may lead to cosmic doomsday when all the astronomical objects will be ripped apart. It is evident that domain of in NHDE is consistent with the observational data of WMAP5 which establishes range of [41].

Figure 15: Evolution trajectories of EoS parameter in NHDE for different values of parameters with . The dot denotes the present day, and star represents the CDM model.

The evolution of is represented in Figure 16 which confirms the behavior of . The curve for assures the CDM model with . The transition from deceleration to accelerated epoch can be seen from this plot, and the values of redshift at the transition point are consistent with the observational results [42, 43]. The plot of statefinder diagnostic in NHDE for different values of parameters is shown in Figure 17. The dot represents the fix point (i.e., the de Sitter phase), and all the curves pass through this point.

Figure 16: Evolution trajectories of in NHDE for different values of parameters with . The dot denotes the present day, and star represents the CDM model.
Figure 17: Evolution trajectories of statefinder diagnostic in NHDE for different values of parameters with .

4. Conclusions

The theory stands as one of the prosperous contexts to describe the cosmic evolution and the present day observational consequences. This theory appears to be a potential candidate in explaining the late time accelerated expansion. A profound model which can explain the cosmic evolution in a definite way is still under consideration. The cosmological reconstruction of gravity has been explored in [2934], and the issue of which approach should be used is still alive. In [3234], function corresponding to a class of HDE models has been constructed by assuming some ansatz for the scale factor in FRW background. A more effective scheme to reconstruct theory from the given evolution history is developed by Capozziello et al. [29]. In this scheme, the significant thing is that we can develop the correspondence of theory to the given DE model by using the expression of respective . As a result, one can find the theory which explains the same dynamics (i.e., the cosmic evolution) as predicted by the given DE model. Now, it is of interest to consider the modified HDE models and address the intrinsic degeneracy among the theory and DE models. We find that predictions of both candidates ( theory and DE models) reconcile as they represent distinct features of the same picture.

In this work, we have reconstructed the function according to NADE and NHDE in flat FRW geometry. The numerical reconstruction scheme is applied to obtain the evolution trajectories of in different scenarios. In this reconstruction procedure, the Hubble parameter plays a significant role as we transform all quantities in terms of and . We summarize our results as follows.(i)For NADE, is given in terms of , so we solve the system of evolution equations for both and . The results are shown in Figures 1 and 2 which are consistent with the constructed functions in the literature [2931]. In comparison with HDE, the future variation of and shows identical behavior for different values of . We can say that the behavior of suggests the de Sitter phase in late time evolution of the universe. The cosmological parameters have been explored in NADE for to make sure the evolution of . Figures 58 evidently show that NADE favors the quintessence regime, and in future evolution, it may end up with the de Sitter phase. Thus, our results for reconstructed are consistent with the independent evolution of NADE. We would like to emphasize that we have taken significantly different values of , but all of these contribute similar results. (ii)In case of HDE with Granda-Oliveros cutoff, the Hubble parameter in the form is directly used in numerical calculations. We have shown the function in and planes in Figure 9. These curves seem to be identical for different values of parameters , and slight difference is found for plane which is shown in Figure 10. Further, we probe the future evolution of and obtain distinct variations accordingly as . The future evolution of in Figures 1214 evidently shows the role of parameters . These plots represent distinct features of which have been later confirmed by the evolution trajectories of and in Figures 15 and 16. For and , it can be seen that depicts the phantom DE era, and in such case and . For , we have representing the de Sitter phase with and . Thus, our results for the function corresponding to NHDE coincide with that of cosmographic parameters.

It is to be noted that NADE and NHDE models are developed in the context of general relativity rather than any modified theory such as gravity. We have reconstructed by considering the curvature part as an effective description of these DE models. We also emphasize that this work is more comprehensive when comparing with previous ones as it involves the analysis of cosmological parameters to ensure the evolution of reconstructed function .


Consider the following:


The authors would like to thank the Higher Education Commission, Islamabad, Pakistan for its financial support through the Indigenous Ph.D. 5000 Fellowship Program Batch-VII.


  1. S. Perlmutter, G. Aldering, and G. Goldhaber, “Measurements of and Λ from 42 high-redshift supernovae,” Astrophysical Journal, vol. 517, p. 565, 1999. View at Publisher · View at Google Scholar
  2. D.N. Sperge, L. Verde, and H. V. Peiris, “First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: determination of cosmological parameters,” The Astrophysical Journal, vol. 148, pp. 175–194, 2003.
  3. M. Tegmark, M. A. Strauss, M. R. Blanton, et al., “Cosmological parameters from SDSS and WMAP,” Physical Review D, vol. 69, Article ID 103501, 26 pages, 2004. View at Publisher · View at Google Scholar
  4. A. G. Riess, L.G. Strolger, and S. Casertano, “New Hubble Space Telescope discoveries of type Ia supernovae at z1: narrowing constraints on the early behavior of dark energy,” Astrophysical Journal, vol. 659, p. 98, 2007.
  5. C. Fedeli, L. Moscardini, and M. Bartelmann, “Observing the clustering properties of galaxy clusters in dynamical dark-energy cosmologies,” Astronomy & Astrophysics, vol. 500, p. 667, 2009. View at Publisher · View at Google Scholar
  6. A. G. Cohen, D. B. Kaplan, and A. E. Nelson, “Effective field theory, black holes, and the cosmological constant,” Physical Review Letters, vol. 82, no. 25, pp. 4971–4974, 1999. View at Publisher · View at Google Scholar · View at Zentralblatt MATH · View at MathSciNet
  7. M. Li, “A model of holographic dark energy,” Physics Letters B, vol. 603, p. 1, 2004.
  8. S. D. H. Hsu, “Entropy bounds and dark energy,” Physics Letters B, vol. 594, pp. 13–16, 2004.
  9. H. Wei and R.-G. Cai, “A new model of agegraphic dark energy,” Physics Letters B, vol. 660, pp. 113–117, 2008.
  10. J.-P. Wu, D.-Z. Ma, and Y. Ling, “Quintessence reconstruction of the new agegraphic dark energy model,” Physics Letters B, vol. 663, pp. 152–159, 2008.
  11. L.-L. Zhang and X.-Q. Liu, “Explicit solutions of (2+1)-dimensional canonical generalized KP, KdV, and (2+1)-dimensional Burgers equations with variable coefficients,” Communications in Theoretical Physics, vol. 52, no. 5, pp. 784–790, 2009. View at Publisher · View at Google Scholar · View at MathSciNet
  12. M. Jamil and E. N. Saridakis, “New agegraphic dark energy in Hořava-Lifshitz cosmology,” Journal of Cosmology and Astroparticle Physics, vol. 07, article 028, 2010.
  13. L. N. Granda and A. Oliveros, “Infrared cut-off proposal for the holographic density,” Physics Letters B, vol. 669, pp. 275–277, 2008.
  14. L. N. Granda and A. Oliveros, “New infrared cut-off for the holographic scalar fields models of dark energy,” Physics Letters B, vol. 671, pp. 199–202, 2009.
  15. M. Sharif and A. Jawad, “Cosmological evolution of interacting new holographic dark energy in non-flat universe,” The European Physical Journal C, vol. 72, p. 2097, 2012.
  16. T. P. Sotiriou and V. Faraoni, “f(R) theories of gravity,” Reviews of Modern Physics, vol. 82, pp. 451–497, 2010.
  17. A. De Fe-lice and S. Tsujikawa, “f(R) theories,” Living Reviews in Relativity, vol. 13, article 3, 2010.
  18. M. Sharif and M. Zubair, “Evolution of the universe in inverse and lnf(R) gravity,” Astrophysics and Space Science, vol. 342, pp. 511–520, 2012.
  19. K. Bamba, S. Capozziello, S. Nojiri, and S. D. Odintsov, “Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests,” Astrophysics and Space Science, vol. 342, no. 1, pp. 155–228, 2012.
  20. T. Harko, F. S. N. Lobo, S. Nojiri, and S. D. Odintsov, “f(R,T) gravity,” Physical Review D, vol. 84, Article ID 024020, 11 pages, 2011.
  21. M. Sharif and M. Zubair, “Thermodynamics in f(R,T) theory of gravity,” Journal of Cosmology and Astroparticle Physics, vol. 03, article 028, 2012.
  22. M. Sharif and M. Zubair, “Erratum: Thermodynamics in f(R,T) theory of gravity,” Journal of Cosmology and Astroparticle Physics, vol. 05, article E01, 2012.
  23. M. Sharif and M. Zubair, “Anisotropic universe models with perfect fluid and scalar field in f(R,T) gravity,” Journal of the Physical Society of Japan, vol. 81, Article ID 114005, 2012.
  24. M. Sharif and M. Zubair, “Energy conditions constraints and stability of power law solutions in f(R,T) gravity,” Journal of the Physical Society of Japan, vol. 82, Article ID 014002, 2013.
  25. M. Sharif and M. Zubair, “Cosmology of holographic and new age-graphic f(R, T) models,” Journal of the Physical Society of Japan, vol. 82, Article ID 064001, 2013.
  26. M. Sharif and M. Zubair, “Thermodynamic behavior of particular f(R, T) gravity models,” Journal of Experimental and Theoretical Physics, 2013.
  27. G. Cognola, E. Elizalde, S. Nojiri, S. D. Odintsov, and S. Zerbini, “Dark energy in modified Gauss-Bonnet gravity: late-time acceleration and the hierarchy problem,” Physical Review D, vol. 73, Article ID 084007, 16 pages, 2006.
  28. M. Sharif and G. Abbas, “Dynamics of shearfree dissipative collapse in f(G) gravity,” Journal of the Physical Society of Japan, vol. 82, Article ID 034006, 2013.
  29. S. Capozziello, V. F. Cardone, and A. Troisi, “Reconciling dark energy models with f(R) theories,” Physical Review D, vol. 71, Article ID 043503, 2005.
  30. X. Wu and Z.-H. Zhu, “Reconstructing f(R) theory according to holographic dark energy,” Physics Letters B, vol. 660, pp. 293–298, 2008.
  31. C.-J. Feng, “Reconstructing f(R) theory from Ricci dark energy,” Physics Letters B, vol. 676, p. 168, 2009.
  32. M. R. Setare, “Holographic modified gravity,” International Journal of Modern Physics D, vol. 17, pp. 2219–2228, 2008.
  33. M. R. Setare, “New agegraphic dark energy in f(R) gravity,” Astrophysics and Space Science, vol. 326, pp. 27–31, 2010.
  34. K. Karami and M. S. Khaledian, “Reconstructing f(R) modified gravity from ordinary and entropy-corrected versions of the holographic and new agegraphic dark energy models,” Journal of High Energy Physics, article 86, 2011.
  35. H. Wei and R.-G. Cai, “Cosmological constraints on new agegraphic dark energy,” Physics Letters B, vol. 663, pp. 1–6, 2008.
  36. J.-F. Zhang, Y.-H. Li, and X. Zhang, “A global fit study on the new agegraphic dark energy model,” The European Physical Journal C, vol. 73, article 2280, 2013.
  37. V. Sahni, T. D. Saini, A. A. Starobinsky, and U. Alam, “Statefinder—a new geometrical diagnostic of dark energy,” JETP Letters, vol. 77, no. 5, pp. 201–206, 2003.
  38. V. Sahni, T. D. Saini, A. A. Starobinsky, and U. Alam, “Statefinder: a new geometrical diagnostic of dark energy,” Pis'ma v Zhurnal Eksperimental'noi i Teoreticheskoi Fiziki, vol. 77, pp. 249–253, 2003.
  39. Y. Wang and L. Xu, “Current observational constraints to the holographic dark energy model with a new infrared cutoff via the Markov chain Monte Carlo method,” Physical Review D, vol. 81, Article ID 083523, 2010.
  40. H. Wei, R. G. Cai, and D. F. Zeng, “Hessence: a new view of quintom dark energy,” Classical and Quantum Gravity, vol. 22, article 3189, 2005.
  41. E. Komatsu, J. Dunkley, M. R. Nolta, et al., “five-year wilkinson microwave anisotropy probe* observations: cosmological interpretation,” Astrophysical Journal, vol. 180, article 330, 2009.
  42. Y.-Z. Ma, “Variable cosmological constant model: the reconstruction equations and constraints from current observational data,” Nuclear Physics B, vol. 804, pp. 262–285, 2008.
  43. R. A. Daly, S. G. Djorgovski, K. A. Freeman, et al., “Improved constraints on the acceleration history of the universe and the properties of the dark energy,” The Astrophysical Journal, vol. 677, no. 1, pp. 1–11, 2008. View at Publisher · View at Google Scholar