Modelling the current accelerated expansion of the Universe with Holographic Dark Energy

Modelling the current accelerated expansion of the Universe with Holographic Dark Energy

Carlos Rodriguez-Benites    Mauricio Cataldo    Antonella Cid and Carlos Ríos Departamento de Física, Grupo Cosmología y Partículas Elementales, Universidad del Bío-Bío, Casilla 5-C, Concepción, Chile.
Departamento de Enseñanza de las Ciencias Básicas, Universidad Católica del Norte, Larrondo 1281, Coquimbo, Chile.
crodriguez@ubiobio.cl
Abstract

In this work we explore a Holographic Dark Energy Model in a flat Friedmann-Lemaître-Robertson-Walker Universe, which contains baryons, radiation, cold dark matter and dark energy within the framework of General Relativity. Furthermore, we consider three types of phenomenological interactions in the dark sector. With the proposed model we obtained the algebraic expressions for the cosmological parameters of our interest: the deceleration and coincidence parameters. Likewise, we graphically compare the proposed model with the CDM model.

1 Introduction

Nowadays it is well known that cosmological models must describe an accelerated expansion of the Universe at the present era [1, 2, 3]. To achieve this, sources of matter capable of generating this acceleration are considered, which are commonly dubbed dark energy [4].

A cosmological constant is an important candidate for dark energy providing a good explanation for the current acceleration. But the cosmological constant faces some problems [5, 6] such as, the mismatch between the expected value of the vacuum energy density and the energy density of the cosmological constant, and the lock of an explanation of why densities of dark energy and dark matter are of same order at present while they evolve in rather different ways. So, as an alternative, dynamical dark energy models have been proposed and analyzed in the literature. Among these, Holographic Dark Energy Models [7, 8, 9, 10, 11, 12] are interacting, because the originate from the holographic principle [13]. The holographic principle asserts that the number of relevant degrees of freedom of a system dominated by gravity must vary along with the area of the surface bounding the system [14]. According to this principle, the vacuum energy density can be bounded [15] as , where is the dark energy density (the vacuum energy density), is the reduced Planck mass, and is the size of the region (i.e IR cutoff). This bound implies that, the total energy inside a region of size , should not exceed the mass of a black hole of the same size. From effective quantum field theory, an effective IR cutoff can saturate the length scale, so that the dark energy density can be written as  [16], where is a dimensionless parameter, and the factor is for mathematical convenience. In the Holographic Ricci Dark Energy Model, is given by the average radius of the Ricci scalar curvature , so in this case the density of the Holographic Dark Energy (hereafter, abbreviated as HDE) is .

In a spatially flat universe, the Ricci scalar of the spacetime is given by , where is the Hubble expansion rate of the universe in terms of the scale factor , where the dot denotes the derivative with respect to the cosmic time . In this sense, the authors of reference [7] introduced the following generalization:

(1)

where and are constants to be determined. This model works fairly well in fitting the observational data, and it is a good candidate to alleviate the cosmic coincidence problem [8, 9, 10, 11, 17].

2 Basic Equations

In the framework of General Relativity we consider a homogeneous, isotropic and flat universe scenario through the Friedmann-Lemaître-Robertson-Walker (FLRW) metric [18]

(2)

where are comoving coordinates. Friedmann’s equations in this context are written as

(3)
(4)

where is the total energy density, is the total pressure and is assumed. On the other hand, the conservation of the total energy-momentum tensor is given by [18]

(5)

3 Holographic Dark Energy Model

We study a scenario that contains baryons, radiation, cold dark matter and HDE, i.e. and . In addition, we consider a barotropic equation of state for the fluids, with , , and . By including a phenomenological interaction in the dark sector, we split the conservation equation (5) in the following equations

(6)

where prime denotes a derivative with respect to and represents the interaction function between cold dark matter and the HDE. From Eqs. (1) and (3) we obtain

(7)

Given that radiation and baryons are separately conserved, we have and . From here it is easy to realize that and .

On the other hand, in the study of HDE scenarios usually it is only considered the dark sector, since these predominate in the current universe. Also, it is possible to analyze a HDE scenario with two different approaches, the first one considers a variable state parameter for the HDE or assuming a parameterization as shown in [11], while the second approach considers an interaction term between the dark components [8, 12, 19]. We work in the last approach.

For convenience, we denote the energy density of the dark sector as . Then, by combining equations (6) - (7) we obtain

(8)

where the submipt denotes a current value. Notice that the eq. (8) can be easily solve when . In this work we consider the following types of linear interactions [20, 21, 22]: , , and .

3.1 The energy density of the dark sector

We can convenient rewrite eq. (8) as

(9)

including the three interaction types of our interest where the values of the constants , , and are shown in Table 1. The general solution of eq. (9) is:

(10)

where the integration constants and are given by

(11)

where , , and are the current values of the Hubble parameter, the density parameters for dark matter and HDE (i.e. with ), respectively. The coefficients in eq. (10) are and , as well as .

Table 1: Definition of the constants , , and in terms of the model’s parameters for the studied interactions.

3.2 The state parameter of the HDE

The state parameter of the HDE corresponds to the ratio . Using the expression (7) in eq. (6), and the linear interactions , we find

(12)

where , , and the constant coefficients are shown in table 2.

Table 2: Definition of the constants , , and in terms of the model’s parameters for the studied interactions.

In the limit to the future, , the expression (12) remains as for , while for , we have .

3.3 The coincidence and deceleration parameters

To examine the problem of cosmological coincidence, we define . Then, using , together with the expression (7), we find

(13)

Then, for all our interactions we get , a constant that depends on the interaction parameters, where for .

On the other hand, the deceleration parameter is a dimensionless measure of the cosmic acceleration in the evolution of the universe. It is defined by  [18]. Using (10), we obtain

(14)
Figure 1: (a) Evolution of coincidence parameter as a function of redshift . (b) Evolution of deceleration parameter as a function of redshift . In the figures, represents current time.

In Fig. 1 we show the evolution of the coincidence and deceleration parameters in term of the redshift , where . We use the following values for the parameters [3]: , , , , km s Mpc, and . In addition, and  [21, 22] are considered. The blue line represents CDM, the orange line the model with and the green line the model with . We note that the HDE models resemble the CDM model, in the evolution of both parameters. Besides, in the cases shown for the HDE models with interaction and , the problem of cosmological coincidence is alleviated, given that the coincidence parameter tend asymptotically to a positive constant.

4 Final Remarks

A theoretical model was developed according to the current components of the Universe, such as baryons, radiation, cold dark dark and HDE, with interaction in the dark sector, obtaining for the HDE, the functions , and . The proposed model was compared graphically with CDM, using referential values for the HDE parameters and the given interactions.

In the near future we expect to contrast the present scenarios with the observational data (SNe Ia, CC, BAO, CMB), using Bayesian statistics.

Acknowledgments

This research was supported by Universidad del Bío-Bío through “Beca de Postgrado”, and research projects DIUBB 181907 4/R (MC) and GI 172309/C (MC, AC).

References

References

  • [1] A. G. Riess et al. [Supernova Search Team], Astron. J. 116, 1009 (1998) [astro-ph/9805201].
  • [2] S. Perlmutter et al. [Supernova Cosmology Project Collaboration], Astrophys. J. 517, 565 (1999) [astro-ph/9812133].
  • [3] P. A. R. Ade et al. [Planck Collaboration], Astron. Astrophys. 594, A13 (2016) [arXiv:1502.01589 [astro-ph.CO]].
  • [4] J. Weller and A. M. Lewis, Mon. Not. Roy. Astron. Soc. 346, 987 (2003) [astro-ph/0307104].
  • [5] E. J. Copeland, M. Sami and S. Tsujikawa, Int. J. Mod. Phys. D 15, 1753 (2006) [hep-th/0603057].
  • [6] A. G. Riess et al., Astrophys. J. 826, no. 1, 56 (2016) [arXiv:1604.01424 [astro-ph.CO]]; A. G. Riess et al., Astrophys. J. 730, 119 (2011) Erratum: [Astrophys. J. 732, 129 (2011)] [arXiv:1103.2976 [astro-ph.CO]].
  • [7] L. N. Granda and A. Oliveros, Phys. Lett. B 669, 275 (2008) [arXiv:0810.3149 [gr-qc]].
  • [8] C. Gao, F. Wu, X. Chen and Y. G. Shen, Phys. Rev. D 79, 043511 (2009) [arXiv:0712.1394 [astro-ph]]; X. Zhang, Phys. Rev. D 79, 103509 (2009) [arXiv:0901.2262 [astro-ph.CO]]; C. J. Feng and X. Zhang, Phys. Lett. B 680, 399 (2009) [arXiv:0904.0045 [gr-qc]]; T. F. Fu, J. F. Zhang, J. Q. Chen and X. Zhang, Eur. Phys. J. C 72, 1932 (2012) [arXiv:1112.2350 [astro-ph.CO]].
  • [9] S. del Campo, J. C. Fabris, R. Herrera and W. Zimdahl, Phys. Rev. D 83, 123006 (2011) [arXiv:1103.3441 [astro-ph.CO]].
  • [10] S. Lepe and F. Pena, Eur. Phys. J. C 69, 575 (2010) [arXiv:1005.2180 [hep-th]].
  • [11] F. Arevalo, P. Cifuentes, S. Lepe and F. Peña, Astrophys. Space Sci. 352, 899 (2014) [arXiv:1308.5007 [gr-qc]].
  • [12] L. P. Chimento, M. I. Forte and M. G. Richarte, AIP Conf. Proc. 1471, 39 (2012) [arXiv:1206.0179 [gr-qc]].
  • [13] J. M. Maldacena, Int. J. Theor. Phys. 38, 1113 (1999) [Adv. Theor. Math. Phys. 2, 231 (1998)] [hep-th/9711200]; W. Fischler and L. Susskind, hep-th/9806039. R. Bousso, Rev. Mod. Phys. 74, 825 (2002) [hep-th/0203101].
  • [14] G. ’t Hooft, Conf. Proc. C 930308, 284 (1993) [gr-qc/9310026]; L. Susskind, J. Math. Phys. 36, 6377 (1995) [hep-th/9409089]; J. D. Bekenstein, Phys. Rev. D 49, 1912 (1994) [gr-qc/9307035].
  • [15] A. G. Cohen, D. B. Kaplan and A. E. Nelson, Phys. Rev. Lett. 82, 4971 (1999) [hep-th/9803132].
  • [16] M. Li, Phys. Lett. B 603, 1 (2004) [hep-th/0403127].
  • [17] T. K. Mathew, J. Suresh and D. Divakaran, Int. J. Mod. Phys. D 22, 1350056 (2013) [arXiv:1207.5886 [astro-ph.CO]]; P. Pankunni and T. K. Mathew, Int. J. Mod. Phys. D 23, 1450024 (2014) [arXiv:1309.3136 [astro-ph.CO]].
  • [18] B. Ryden, Introduction to Cosmology, Ohio State University Press, (2006).
  • [19] S. Chattopadhyay and A. Pasqua, Indian J. Phys. 87, 1053 (2013).
  • [20] M. Cataldo, F. Arevalo and P. Minning, JCAP 1002, 024 (2010) [arXiv:1002.3415 [astro-ph.CO]].
  • [21] F. Arevalo, A. Cid and J. Moya, Eur. Phys. J. C 77, no. 8, 565 (2017) [arXiv:1610.09330 [astro-ph.CO]].
  • [22] A. Cid, B. Santos, C. Pigozzo, T. Ferreira and J. Alcaniz, arXiv:1805.02107 [astro-ph.CO].
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 ...
366512
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