Advances in High Energy Physics

Volume 2013 (2013), Article ID 143195, 11 pages

http://dx.doi.org/10.1155/2013/143195

Research Article

in Holographic and Agegraphic Dark Energy Models and the Generalized Uncertainty Principle

Barun Majumder

Indian Institute of Technology Gandhinagar, Ahmedabad, Gujarat 382424, India

Received 16 April 2013; Accepted 16 July 2013

Academic Editor: George Siopsis

Copyright © 2013 Barun Majumder. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Abstract.

We studied a unified approach with the holographic, new agegraphic, and dark energy model to construct the form of which in general is responsible for the curvature driven explanation of the very early inflation along with presently observed late time acceleration. We considered the generalized uncertainty principle in our approach which incorporated the corrections in the entropy-area relation and thereby modified the energy densities for the cosmological dark energy models considered. We found that holographic and new agegraphic gravity models can behave like phantom or quintessence models in the spatially flat FRW universe. We also found a distinct term in the form of which goes as due to the consideration of the GUP modified energy densities. Although the presence of this term in the action can be important in explaining the early inflationary scenario, Capozziello et al. recently showed that leads to an accelerated expansion, that is, a negative value for the deceleration parameter which fits well with SNeIa and WMAP data.

1. Introduction

Observations of type IA supernovae confirm that our present universe is expanding at an accelerating rate [1]. Present observational cosmology has provided enough evidence in favour of the accelerated expansion of the universe [2–4]. Theoretical aid came in the form of exotic dark energy (DE) which can generate sufficient negative pressure and is believed to account nearly 70% of present energy of the universe. Researchers in theoretical physics have proposed many DE models but they face problems while incorporating the history of the universe. The models generally have many free parameters and face serious constraints from observational data. Recent reviews [5–9] are useful for a brief knowledge of DE models.

The holographic DE is one of the promising DE models and the model is based on the holographic principle [10–14]. Bekenstein's entropy bound suggests that quantum field theory breaks down at large volumes. This can be reconciled by using a relation between UV and IR cut-offs such that , where is the reduced Planck Mass (). In this situation an effective local quantum field theory will give a good approximate description [15]. The holographic DE was first proposed in [16] following the line of [15] where the infrared cut-off is taken to be the size of event horizon for DE. The problem of cosmic coincidence can be resolved by the inflationary paradigm with minimal e-foldings in this model. Later this holographic DE was studied in detail by many authors [17–26]. Clearly it can be mentioned that black hole entropy bound played an important role in the interpretation of holographic dark energy model. Various theories of quantum gravity (e.g., [27–33]) have predicted the following form for the entropy of a black hole:

is a model dependent parameter and is the Planck length. Many researchers have expressed a vested interest in fixing (the coefficient of the subleading logarithmic term) [27]. Recent rigorous calculations of loop quantum gravity predict the value of to be −1/2 [33]. A entropy corrected holographic DE model (ECHDE) was proposed recently in [34] where the inflation was driven by ECHDE. The curvature perturbation may be generated through the curvaton and the only requirement remain as [35, 36].

Another promising DE candidate is the agegraphic DE and was proposed in [37]. Considering the quantum fluctuations of spacetime Károlyházy and his collaborators [38–40] argued that in Minkowski spacetime any distance cannot be known to a better accuracy than , where is the reduced Planck time. Based on the arguments of Károlyházy it can be shown that for Minkowski spacetime the energy density of metric fluctuations is given by [41, 42]. The agegraphic DE model considers spacetime and matter field fluctuations responsible for DE. If conformal time is considered in place of the age of the universe the model can describe the matter dominated epoch [43] with a natural solution to the coincidence problem [44] and is known as the new agegraphic DE model. The conformal time is defined by , where is the cosmic time and the scale factor. Many authors did some detailed study of this new agegraphic DE model [45–48].

Also we have other possible explanations for the cosmic acceleration, the different being the approach with gravity, where is the scalar curvature. Other forms of along with in the Lagrangian can explain the observed acceleration without considering other additional components (the review [49] is useful). Among other existing theories gravity models can be shown to be compatible with a matter dominated epoch transiting into an accelerating phase [50]. Also the forms of with positive powers of curvature support the inflationary epoch and forms with negative powers of curvature serving as the effective DE responsible for cosmic acceleration and compatible with solar system experiments [51]. Also it is worth mentioning that these models face some challenges in the line of argument discussed in [52–56].

The idea that the uncertainty principle could be affected by gravity was given by Mead [57]. In the regime when the gravity is strong enough, conventional Heisenberg uncertainty relation is no longer satisfactory (though approximately but perfectly valid in low gravity regimes). Later modified commutation relations between position and momenta, commonly known as generalized uncertainty principle (GUP), were given by candidate theories of quantum gravity (String Theory, doubly special relativity theory and Black Hole Physics) with the prediction of a minimum measurable length [58–67]. Similar kind of commutation relation can also be found in the context of Polymer Quantization in terms of polymer mass scale [68]. Importance of the GUP can also be realized on the basis of simple gedanken experiments without any reference to a particular fundamental theory [65, 66]. So we can think of the GUP as a model-independent concept, ideally perfect for the study of black hole entropy. The authors in [69] proposed a GUP which is consistent with DSR theory, string theory, and black hole physics. This is approximately covariant under DSR transformations but not Lorentz covariant [67]. With the GUP as proposed by the authors in [69] we can arrive at the corrected entropy-area relation for a black hole which can be written in the following expansive form [70, 71]:

In this paper we will try to predict the form of in holographic and new agegraphic DE models in the light of the generalized uncertainty principle. In [72] it has been argued that the holographic theory does not retain its good features by considering minimal length in quantum gravity. But here we will try to avoid the issue and hope to present the discussion in some future work. We will use (2) to calculate the energy density for the models. Later we will construct the form of and the equation of state parameter for each of these DE models. Although an earlier attempt is present in the literature for the reconstruction of [73] but we will later conclude with a brief comparison of the results.

2. from Holographic DE Model with GUP

In gravity the action is written as [74–76]

The considerations lie in the fact that the higher order modifications of the Ricci curvature in the form of or could give rise to inflation at the very early universe. The term does not lead to any new kind of inflation different from that produced by the term since the combination does not contribute to the de Sitter solution at all. So this leads to a notion that whether inverse powers in dominant in late time universe can give an explanation to the recent predicted acceleration of the universe. But this type of models faces problems of stability [77]. The variation of the action with respect to the metric gives the field equations as

where

Here , is the Ricci tensor, is the energy momentum tensor of matter, and denotes the curvature contribution.

For a spatially flat FRW universe the modified Friedmann equation can be written as

where

Here the Hubble parameter is and the overdot denotes derivative with respect to cosmic time . We can show that the curvature contribution will have its own equation of state and it can be written as [78]

In gravity theories we usually encounter three types of scale factors for accelerating and inflationary cosmological solutions. We will follow the details of [73, 79]. Here we will study phantom, quintessence, and de Sitter scale factors which are given by

With the phantom scale factor and (9) we get

and also

Recent observations constrain the value of for the phantom scale factor to be [80]. Similarly with the quintessence scale factor and (9) we get

and also

For this quintessence scale factor the value of is very close to unity [80]. For de Sitter solution we have . This scale factor is used to describe the early inflationary scenario. For this case we get

Now we will try to evaluate the form of for each of the scale factor mentioned above in the light of the generalized uncertainty principle (GUP). For our purpose we need to solve (7) and we borrow the energy density from the holographic and agegraphic dark energy models, respectively.

Considering the leading order terms of (2) and following the arguments of [34, 81] we can write the GUP motivated energy density for the holographic DE model as

Here , and are constants and is the future event horizon. If we get the usual holographic DE model. Though is a constant, its value can be constrained from the latest observational data [82]. The future event horizon is defined as

For the phantom scale factor the future event horizon is

Putting the value of in (17) we get the form of energy density as

Now (7) can be written in terms of as

where . This equation is a nonhomogeneous Euler differential equation and the solution can be written as

where

with as integration constants whose value can be predicted by the boundary conditions. The boundary conditions are

where is the present value of which is a small constant. The value of is of the order of . If we apply the boundary conditions we get the values of as

In general the equation of state of (10) will be a function of and hence time in this case and so it can explain the transition from quintessence () to phantom dominated regime () as predicted by recent observations [83–85]. If we see (22) we can infer that there is a contribution from . This is interesting from the fact that we can have contributions from fractional powers of . We will discuss this in a later part of this study.

For the quintessence scale factor the future event horizon is at

with the condition . Putting the value of from (26) in (17) we get the form of energy density as

So for the quintessence scale factor equations (14) and (15) we can rewrite (7) with (27) as

where . Similarly like the phantom case the solution can be written as

where

The boundary conditions will give

For the scale factor in de Sitter space is constant. The future event horizon is located at

where is given by (16). So we can write the GUP motivated energy density from (17) as

So (7) takes the form

The solution of this equation can be written in the form

where is the arbitrary integration constant to be fixed by boundary conditions. The GUP motivated terms in are important for inflationary scenario. We have instances for the term in the literature to explain early time inflation [74] as a curvature driven phenomenon. Here we have a new term in which can be important for curvature driven inflation. We will discuss more about this term later in the Discussion section.

3. from New Agegraphic DE Model with GUP

With the corrections due to the generalized uncertainty principle to the entropy area relation we can frame the energy density of the new agegraphic DE model [34, 81] as

where is the conformal time. will give back the usual new agegraphic DE model. The parameter is constrained by present observations and its best fit value is around with uncertainty [44]. The numerical factor was introduced for a parameterization of some uncertainties such as the effect of curved spacetime, (as the Károlyházy relation considered only the metric quantum fluctuations of Minkowski spacetime) and the species of quantum fields in the universe.

For the phantom scale factor the conformal time can be evaluated as

Substituting this in (36) we get

Solving the inhomogeneous Euler differential equation (7) with (38) we get the form of as

where

The boundary conditions will give

In general the equation of state of (10) will be a function of and hence time in this case and so it can explain the transition from quintessence () to phantom dominated regime () as predicted by recent observations [83–85]. For the quintessence scale factor (11) the conformal time can be evaluated with (14) and (15) as

For a real finite conformal time it is necessary to have . Substituting this in (36) we get

Solving the inhomogeneous Euler differential equation (7) with (43), (14), and (15) we get the form of as

where

The boundary conditions and will give

For the scale factor with (de Sitter) we write the conformal time as

Here we have set the upper limit of the integration to to express in terms of . The relevant modification to the energy density (36) will be

The solution of (7) with (47) and (48) yields the form of as

where is the integration constant to be fixed with boundary conditions. Here also like the holographic DE model we have a new term in which can be important for curvature driven inflation.

4. Discussion

In this study we considered the generalized uncertainty principle motivated forms of the holographic and the new agegraphic DE models to reconstruct the form of suitable to explain the unification of early time inflation and late time acceleration. The idea that the Heisenberg uncertainty principle could be affected by gravity was given by Mead [57]. In the regime when the gravity is strong enough, conventional Heisenberg uncertainty relation is no longer satisfactory (though approximately but perfectly valid in low gravity regimes). Modified commutation relations between position and momenta, commonly known as the generalized uncertainty principle (or GUP), were given by candidate theories of quantum gravity like string theory, doubly special relativity, and black hole physics with the prediction of a minimum measurable length. Importance of the GUP can also be realized on the basis of simple gedanken experiments without any reference of a particular fundamental theory [65, 66]. So we can think of the GUP as a model-independent concept suitable for the study of black hole entropy at least phenomenologically.

According to the holographic principle the number of degrees of freedom of a bounded system should be finite and is related to the area of its boundary. As an application of the principle the upper bound of the entropy of the universe can be obtained. The total energy of a system of size should not exceed the mass of a black hole of the same size, otherwise it would decay into a black hole. The saturation of the inequality means where is the reduced Planck Mass (). The UV cut-off is related to the vacuum energy and the IR cut-off is related to the large scale of the universe. The holographic dark energy scenario is viable if we set the IR cut-off by the future event horizon and also make a concrete prediction about the equation of state of the DE [16]. On the other hand the new agegraphic DE model is based on the Károlyházy relation which considers energy density of quantum fluctuations of the metric and matter in the universe. The energy density of the new agegraphic DE model has the same form as the holographic dark energy but the conformal time takes care of the IR cut-off instead of considering the future event horizon of the universe. The model not only accounts the observed value of DE in the universe but also predicts an accelerated expansion. Among various theoretical approaches to explain the present cosmic accelerated expansion of the universe only the holographic and the new agegraphic DE model is somehow based on the entropy-area relation. The entropy-area relation on the other hand can have quantum corrections through various approaches of quantum gravity.

As no single theoretical proposal for DE enjoys a pronounced supremacy over the others in terms of having a strong field theoretic support as well as being able to explain all the present observational data. This state of art explores another possibility of whether geometry in its own right could explain the presently observed accelerated expansion. The idea stems from the fact that higher order modifications of the Ricci curvature along with in the Einstein-Hilbert action could generate inflation in the very early universe. As the curvature is expected to fall off with the cosmic evolution it is then obvious whether inverse powers of in the action dominant during the later stages could drive a late time acceleration. In general this alternative theory is coined as gravity.

In this paper we studied a unified approach with the holographic, new agegraphic, and DE model to construct the form of which in general is responsible for the curvature driven explanation of the very early inflation along with presently observed late time acceleration. We considered the generalized uncertainty principle in our approach which incorporated the corrections in the entropy area relation which thereby modified the energy densities for the cosmological DE models considered here. In the context of modified theories of gravity we should be cautious with the Wald entropy [86, 87] and not the Bekenstein-Hawking entropy. The Wald entropy is defined in terms of quantities on the Killing horizon and it depends on the variation of the Lagrangian density of the modified gravity theory with respect to the Riemann tensor. The Wald entropy is a local quantity and in gravity it is given by [88]. However, here we have just reconstructed from the energy densities of other DE models. We found that the GUP motivated holographic and new agegraphic gravity models can behave like phantom or quintessence models in the spatially flat FRW universe. A similar study was also carried out by authors in [73]. We reproduced all the result and conclusion of [73] but in addition we also found a distinct term in the form of which goes as due to the consideration of the GUP modified energy densities. This is really very interesting if we consider the phenomenological consequence of our study. Although the presence of this term in the action can have its importance for inflation, Capozziello et al. [89, 90] introduced an action with and showed that it leads to an accelerated expansion, that is, a negative value for the deceleration parameter for which fits well with SNeIa and WMAP data. Apart from the term we also found the other possible contributions of like and which also have importance in the inflationary scenario. We should also mention here that in the latter case one needs not only quasi-exponential expansion but a metastable (i.e. slowly rolling) one. In gravity this may occur only if is close to over some range of [91].

Acknowledgments

The author was partly supported by the Excellence-in-Research Fellowship of IIT Gandhinagar. The author would like to thank an anonymous referee for enlightening comments which immensely helped in improving the paper.

References

A. G. Riess, A. V. Filippenko, P. Challis, et al., “Observational evidence from supernovae for an accelerating universe and a cosmological constant,” The Astronomical Journal, vol. 116, no. 3, p. 1009, 1998.

S. Perlmutter, G. Aldering, G. Goldhaber et al., “Measurements of Ω and Λ from 42 high-redshift Supernovae,” Astrophysical Journal Letters, vol. 517, no. 2, pp. 565–586, 1999.

P. de Bernardis, P. A. R. Ade, J. J. Bock, et al., “A flat Universe from high-resolution maps of the cosmic microwave background radiation,” Nature, vol. 404, pp. 955–959, 2000.

R. A. Knop, G. Aldering, R. Amanullah, et al., “New constraints on ΩM, ΩΛ, and w from an independent set of 11 high-redshift supernovae observed with the Hubble Space Telescope,” The Astrophysical Journal, vol. 598, no. 1, p. 102, 2003.

V. Sahni and A. A. Starobinsky, “The case for a positive cosmological Lambda-term,” International Journal of Modern Physics D, vol. 9, pp. 373–444, 2000.

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

P. J. E. Peebles and B. Ratra, “The cosmological constant and dark energy,” Reviews of Modern Physics, vol. 75, no. 2, pp. 559–606, 2003.

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

V. Sahni and A. Starobinsky, “Reconstructing dark energy,” International Journal of Modern Physics D, vol. 15, no. 12, pp. 2105–2132, 2006.

P. Hořava and D. Minic, “Probable values of the cosmological constant in a holographic theory,” Physical Review Letters, vol. 85, no. 8, pp. 1610–1613, 2000.

S. Thomas, “Holography stabilizes the vacuum energy,” Physical Review Letters, vol. 89, no. 8, Article ID 081301, 4 pages, 2002.

G. 't Hooft, “Dimensional reduction in quantum gravity,” http://arxiv.org/abs/gr-qc/9310026

L. Susskind, “The world as a hologram,” Journal of Mathematical Physics, vol. 36, no. 11, pp. 6377–6396, 1995.

W. Fischler and L. Susskind, “Holography and cosmology,” http://arxiv.org/abs/hep-th/9806039

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.

M. Li, “A model of holographic dark energy,” Physics Letters B, vol. 603, pp. 1–5, 2004.

K. Enqvist and M. S. Sloth, “Possible connection between the location of the cutoff in the cosmic microwave background spectrum and the equation of state of dark energy,” Physical Review Letters, vol. 93, no. 22, Article ID 221302, 2004.

Q.-G. Huang and Y.-G. Gong, “Supernova constraints on a holographic dark energy model,” Journal of Cosmology and Astroparticle Physics, no. 8, pp. 141–148, 2004.

E. Elizalde, S. Nojiri, S. D. Odintsov, and P. Wang, “Dark energy: vacuum fluctuations, the effective phantom phase, and holography,” Physical Review D, vol. 71, no. 10, Article ID 103504, 8 pages, 2005.

X. Zhang and F.-Q. Wu, “Constraints on holographic dark energy from type Ia supernova observations,” Physical Review D, vol. 72, no. 4, Article ID 043524, 10 pages, 2005.

B. Guberina, R. Horvat, and H. Štefančić, “Hint for quintessence-like scalars from holographic dark energy,” Journal of Cosmology and Astroparticle Physics, no. 5, pp. 1–7, 2005.

J. P. Beltrán Almeida and J. G. Pereira, “Holographic dark energy and the universe expansion acceleration,” Physics Letters B, vol. 636, no. 2, pp. 75–79, 2006.

B. Guberina, R. Horvat, and H. Nikolić, “Dynamical dark energy with a constant vacuum energy density,” Physics Letters B, vol. 636, no. 2, pp. 80–85, 2006.

X. Zhang, “Dynamical vacuum energy, holographic quintom, and the reconstruction of scalar-field dark energy,” Physical Review D, vol. 74, no. 10, Article ID 103505, 7 pages, 2006.

X. Zhang and F.-Q. Wu, “Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations,” Physical Review D, vol. 76, no. 2, Article ID 023502, 8 pages, 2007.

L. Xu, “Holographic dark energy model with Hubble horizon as an IR cut-off,” Journal of Cosmology and Astroparticle Physics, vol. 2009, p. 16, 2009.

R. K. Kaul and P. Majumdar, “Logarithmic correction to the Bekenstein-Hawking entropy,” Physical Review Letters, vol. 84, no. 23, pp. 5255–5257, 2000.

A. J. M. Medved and E. C. Vagenas, “When conceptual worlds collide: the generalized uncertainty principle and the Bekenstein-Hawking entropy,” Physical Review D, vol. 70, no. 12, Article ID 124021, 5 pages, 2004.

S. Das, P. Majumdar, and R. K. Bhaduri, “General logarithmic corrections to black-hole entropy,” Classical and Quantum Gravity, vol. 19, no. 9, pp. 2355–2367, 2002.

M. Domagala and J. Lewandowski, “Black-hole entropy from quantum geometry,” Classical and Quantum Gravity, vol. 21, no. 22, pp. 5233–5243, 2004.

A. Chatterjee and P. Majumdar, “Universal canonical black hole entropy,” Physical Review Letters, vol. 92, no. 14, Article ID 141301, 4 pages, 2004.

G. Amelino-Camelia, M. Arzano, and A. Procaccini, “Severe constraints on the loop-quantum-gravity energy-momentum dispersion relation from the black-hole area-entropy law,” Physical Review D, vol. 70, no. 10, Article ID 107501, 4 pages, 2004.

K. A. Meissner, “Black-hole entropy in loop quantum gravity,” Classical and Quantum Gravity, vol. 21, no. 22, pp. 5245–5251, 2004.

H. Wei, “Effects of transverse field on internal energy and specific heat of a molecular-based materials,” Communications in Theoretical Physics, vol. 52, no. 5, p. 743, 2009.

D. H. Lyth and D. Wands, “Generating the curvature perturbation without an inflaton,” Physics Letters B, vol. 524, pp. 5–14, 2002.

D. H. Lyth, C. Ungarelli, and D. Wands, “Primordial density perturbation in the curvaton scenario,” Physical Review D, vol. 67, no. 2, Article ID 023503, 2003.

R.-G. Cai, “A dark energy model characterized by the age of the universe,” Physics Letters B, vol. 657, no. 4-5, pp. 228–231, 2007.

F. Károlyházy, “Gravitation and quantum mechanics of macroscopic objects,” Il Nuovo Cimento A, vol. 42, no. 2, pp. 390–402, 1966.

F. Károlyházy, A. Frenkel, and B. Lukacs, “On the possibility of observing the eventual breakdown of the superposition principle,” in Physics as Natural Philosophy, A. Shimony and H. Feschbach, Eds., The MIT Press, Cambridge, Mass, USA, 1982.

F. Károlyházy, A. Frenkel, and B. Lukacs, “On the possible role of gravity in the reduction of the wave function,” in Quantum Concepts in Space and Time, R. Penrose and C. J. Isham, Eds., Clarendon Press, Oxford, UK, 1986.

M. Maziashvili, “Space–time in light of Károlyházy uncertainty relation,” International Journal of Modern Physics D, vol. 16, no. 9, p. 1531, 2007.

M. Maziashvili, “Cosmological implications of Károlyházy uncertainty relation,” Physics Letters B, vol. 652, pp. 165–168, 2007.

H. Wei and R.-G. Cai, “A new model of agegraphic dark energy,” Physics Letters B, vol. 660, pp. 113–117, 2008.

H. Wei and R.-G. Cai, “Cosmological constraints on new agegraphic dark energy,” Physics Letters B, vol. 663, pp. 1–6, 2008.

Y.-W. Kim, H. W. Lee, Y. S. Myung, and M.-I. Park, “New agegraphic dark energy model with generalized uncertainty principle,” Modern Physics Letters A, vol. 23, no. 36, p. 3049, 2008.

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.

I. P. Neupane, “A note on agegraphic dark energy,” Physics Letters B, vol. 673, pp. 111–118, 2009.

K. Y. Kim, H. W. Lee, and Y. S. Myung, “Instability of agegraphic dark energy models,” Physics Letters B, vol. 660, pp. 118–124, 2008.

S. Capozziello, “Curvature quintessence,” International Journal of Modern Physics D, vol. 11, no. 4, p. 483, 2002.

S. Capozziello, S. Nojiri, S. D. Odintsov, and A. Troisi, “Cosmological viability of f (R)-gravity as an ideal fluid and its compatibility with a matter dominated phase,” Physics Letters B, vol. 639, no. 3-4, pp. 135–143, 2006.

S. Nojiri and S. D. Odintsov, “Modified gravity with negative and positive powers of curvature: Unification of inflation and cosmic acceleration,” Physical Review D, vol. 68, Article ID 123512, 10 pages, 2003.

L. Amendola, D. Polarski, and S. Tsujikawa, “Are dark energy models cosmologically viable?” Physical Review Letters, vol. 98, no. 13, Article ID 131302, 4 pages, 2007.

L. Amendola, D. Polarski, and S. Tsujikawa, “Power-laws f(R) theories are cosmologically unacceptable,” International Journal of Modern Physics D, vol. 16, no. 10, pp. 1555–1561, 2007.

W. Hu and I. Sabik, “Models of f(R) cosmic acceleration that evade solar system tests,” Physical Review D, vol. 76, Article ID 064004, 13 pages, 2007.

S. A. Appleby and R. A. Battye, “Do consistent models mimic general relativity plus Λ?” Physics Letters B, vol. 654, no. 1-2, pp. 7–12, 2007.

A. A. Starobinsky, “Disappearing cosmological constant in f(R) gravity,” JETP Letters, vol. 86, no. 3, pp. 157–163, 2007.

C. A. Mead, “Possible connection between gravitation and fundamental length,” Physical Review D, vol. 135, pp. B849–B862, 1964.

D. Amati, M. Ciafaloni, and G. Veneziano, “Can spacetime be probed below the string size?” Physics Letters B, vol. 216, no. 1-2, pp. 41–47, 1989.

M. Maggiore, “The algebraic structure of the generalized uncertainty principle,” Physics Letters B, vol. 319, no. 1–3, pp. 83–86, 1993.

S. Hossenfelder, M. Bleicher, S. Hofmann, J. Ruppert, S. Scherer, and H. Stöcker, “Signatures in the Planck regime,” Physics Letters B, vol. 575, no. 1-2, pp. 85–99, 2003.

C. Bambi and F. R. Urban, “Natural extension of the generalized uncertainty principle,” Classical and Quantum Gravity, vol. 25, no. 9, Article ID 095006, 8 pages, 2008.

A. Kempf, G. Mangano, and R. B. Mann, “Hilbert space representation of the minimal length uncertainty relation,” Physical Review D, vol. 52, no. 2, pp. 1108–1118, 1995.

F. Brau, “Minimal length uncertainty relation and the hydrogen atom,” Journal of Physics A, vol. 32, no. 44, pp. 7691–7696, 1999.

J. Magueijo and L. Smolin, “Lorentz invariance with an invariant energy scale,” Physical Review Letters, vol. 88, no. 19, Article ID 190403, 4 pages, 2002.

M. Maggiore, “A generalized uncertainty principle in quantum gravity,” Physics Letters B, vol. 304, pp. 65–69, 1993.

F. Scardigli, “Generalized uncertainty principle in quantum gravity from micro-black hole gedanken experiment,” Physics Letters B, vol. 452, pp. 39–44, 1999.

J. L. Cortés and J. Gamboa, “Quantum uncertainty in doubly special relativity,” Physical Review D, vol. 71, no. 6, Article ID 065015, 4 pages, 2005.

G. M. Hossain, V. Husain, and S. S. Seahra, “Background-independent quantization and the uncertainty principle,” Classical and Quantum Gravity, vol. 27, no. 16, Article ID 165013, 8 pages, 2010.

A. F. Ali, S. Das, and E. C. Vagenas, “Discreteness of space from the generalized uncertainty principle,” Physics Letters B, vol. 678, no. 5, pp. 497–499, 2009.

B. Majumder, “Black hole entropy and the modified uncertainty principle: a heuristic analysis,” Physics Letters B, vol. 703, no. 4, pp. 402–405, 2011.

B. Majumder, “Black hole entropy with minimal length in tunneling formalism,” submitted in General Relativity and Gravitation, http://arxiv.org/abs/1212.6591

A. F. Ali, “Minimal length in quantum gravity, equivalence principle and holographic entropy bound,” Classical and Quantum Gravity, vol. 28, no. 6, Article ID 065013, 10 pages, 2011.

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, vol. 2011, article 86, 2011.

A. A. Starobinsky, “A new type of isotropic cosmological models without singularity,” Physics Letters B, vol. 91, pp. 99–102, 1980.

R. Kerner, “Cosmology without singularity and nonlinear gravitational Lagrangians,” General Relativity and Gravitation, vol. 14, no. 5, pp. 453–469, 1982.

J.-P. Duruisseau and R. Kerner, “The effective gravitational Lagrangian and the energy-momentum tensor in the inflationary universe,” Classical and Quantum Gravity, vol. 3, no. 5, pp. 817–824, 1986.

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.

K. Nozari and T. Azizi, “Phantom-like behavior in -gravity,” Physics Letters B, vol. 680, pp. 205–211, 2009.

S. Nojiri and S. D. Odintsov, “Introduction to modified gravity and gravitational alternative for dark energy,” International Journal of Geometric Methods in Modern Physics, vol. 4, no. 1, pp. 115–145, 2007.

R. Rangdee and B. Gumjudpai, “Tachyonic (phantom) power-law cosmology,” http://arxiv.org/abs/1210.5550

B. Guberina, R. Horvat, and H. Nikolić, “Non-saturated holographic dark energy,” Journal of Cosmology and Astroparticle Physics, no. 1, article 12, 2007.

M. Li, X. -D. Li, S. Wang, and X. Zhang, “Holographic dark energy models: a comparison from the latest observational data,” Journal of Cosmology and Astroparticle Physics, vol. 6, p. 36, 2009.

U. Alam, V. Sahni, and A. A. Starobinsky, “The case for dynamical dark energy revisited,” Journal of Cosmology and Astroparticle Physics, no. 6, pp. 113–128, 2004.

D. Huterer and A. Cooray, “Uncorrelated estimates of dark energy evolution,” Physical Review D, vol. 71, no. 2, Article ID 023506, 5 pages, 2005.

Y. Wang and M. Tegmark, “Uncorrelated measurements of the cosmic expansion history and dark energy from supernovae,” Physical Review D, vol. 71, Article ID 103513, 7 pages, 2005.

R. M. Wald, “Black hole entropy is the Noether charge,” Physical Review D, vol. 48, no. 8, pp. R3427–R3431, 1993.

V. Iyer and R. M. Wald, “Some properties of the Noether charge and a proposal for dynamical black hole entropy,” Physical Review D, vol. 50, no. 2, pp. 846–864, 1994.

R. Brustein, D. Gorbonos, and M. Hadad, “Wald's entropy is equal to a quarter of the horizon area in units of the effective gravitational coupling,” Physical Review D, vol. 79, no. 4, Article ID 044025, 9 pages, 2009.

S. Capozziello, S. Carloni, and A. Troisi, “Quintessence without scalar fields,” Astronomy & Astrophysics, vol. 1, p. 625, 2003.

S. Capozziello, V. F. Cardone, S. Carloni, and A. Troisi, “Curvature quintessence matched with observational data,” International Journal of Modern Physics D, vol. 12, no. 10, pp. 1969–1982, 2003.

S. A. Appleby, R. A. Battye, and A. A. Starobinsky, “Curing singularities in cosmological evolution of F(R) gravity,” Journal of Cosmology and Astroparticle Physics, vol. 2010, no. 6, article 5, 2010.