New holographic reconstruction of scalar-field dark-energy models in the framework of chameleon Brans–Dicke cosmology

The European Physical Journal C, Sep 2014

Motivated by the work of Yang et al. (Mod. Phys. Lett. A 26:191, 2011), we report on a study of the new holographic dark energy (NHDE) model with energy density given by \(\rho _D\!=\!\frac{3\phi ^2}{4\omega }(\mu H^2\!+\!\nu {\dot{H}})\) in the framework of chameleon Brans–Dicke cosmology. We have studied the correspondence between the quintessence, the DBI-essence, and the tachyon scalar-field models with the NHDE model in the framework of chameleon Brans–Dicke cosmology. Deriving an expression of the Hubble parameter \(H\) and, accordingly, \(\rho _D\) in the context of chameleon Brans–Dicke chameleon cosmology, we have reconstructed the potentials and dynamics for these scalar-field models. Furthermore, we have examined the stability for the obtained solutions of the crossing of the phantom divide under a quantum correction of massless conformally invariant fields, and we have seen that the quantum correction could be small when the phantom crossing occurs and the obtained solutions of the phantom crossing could be stable under the quantum correction. It has also been noted that the potential increases as the matter–chameleon coupling gets stronger with the evolution of the universe.

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New holographic reconstruction of scalar-field dark-energy models in the framework of chameleon Brans–Dicke cosmology

Surajit Chattopadhyay 2 Antonio Pasqua 1 Martiros Khurshudyan 0 3 0 Department of Theoretical Physics, Yerevan State University , 1 A. Manookian, Yerevan, Armenia 1 Department of Physics, University of Trieste , Via Valerio, 2, 34127 Trieste, Italy 2 Pailan College of Management and Technology , Bengal Pailan Park, Kolkata 700 104, India 3 Present address: Max Planck Institute of Colloids and Interfaces, Potsdam-Golm Science Park , Am Mhlenberg 1 OT Golm, 14476 Potsdam, Germany Motivated by the work of Yang et al. (Mod. Phys. Lett. A 26:191, 2011), we report on a study of the new holographic dark energy (NHDE) model with energy density given by D = 342 (H 2 + H ) in the framework of chameleon Brans-Dicke cosmology. We have studied the correspondence between the quintessence, the DBI-essence, and the tachyon scalar-field models with the NHDE model in the framework of chameleon Brans-Dicke cosmology. Deriving an expression of the Hubble parameter H and, accordingly, D in the context of chameleon Brans-Dicke chameleon cosmology, we have reconstructed the potentials and dynamics for these scalar-field models. Furthermore, we have examined the stability for the obtained solutions of the crossing of the phantom divide under a quantum correction of massless conformally invariant fields, and we have seen that the quantum correction could be small when the phantom crossing occurs and the obtained solutions of the phantom crossing could be stable under the quantum correction. It has also been noted that the potential increases as the matterchameleon coupling gets stronger with the evolution of the universe. The approaches to account for the late-time cosmic acceleration, which is suggested by the two independent observational signals on distant Type Ia Supernovae (SNeIa) [13], the cosmic microwave background (CMB) temperature anisotropies measured by the WMAP and Planck satellites - [46] and Baryon Acoustic Oscillations (BAO) [7,8], fall into two representative categories: in the first, the concept of dark energy is introduced in the right-hand side of the Einstein equation in the framework of general relativity (for good reviews see [911]), while in the second one the lefthand side of the Einstein equation is modified, leading to a modified gravitational theory (which is well reviewed in [12 15]). In a recent review, Bamba et al. [10] demonstrated that both dark-energy models and modified gravity theories seem to be in agreement with data and hence, unless higher precision probes of the expansion rate and the growth of structure will be available, these two rival approaches could not be discriminated. The physical origin of dark energy (DE) is one of the largest mysteries not only in cosmology but also in fundamental physics [9,1619]. The cosmological constant represents the earliest and the simplest theoretical candidate proposed in order to explain the observational evidence of accelerated expansion. Some tentative deviations from the CDM model may eventually rule out an exact cosmological constant [20,21]. A considerable number of models for DE have been proposed up to now to explain the late-time cosmic acceleration without the cosmological constant. Such models include a canonical scalar field, the so-called quintessence, a non-canonical scalar field such as phantom, tachyon scalar field motivated by string theories, and a fluid with a special equation of state (EoS) called a Chaplygin gas. Other well studied candidates for DE are the k-essence, the quintom and the agegraphic dark energy (ADE) models. Studies on the models previously mentioned include [9,10,22 29]. There also exists a proposal known as holographic dark energy (HDE) proposed by Li [30], following the idea that the short distance cut-off is related to the infrared cut-off and it was assumed in [30] that the infrared cut-off relevant to the dark energy is the size of the event horizon. Some notable works on HDE include [3134]. Furthermore, there exists plethora of literature on HDE in theoretical aspects as well as observational constraints e.g. [3537]. The equation of state (EoS) parameter, defined as wDE = pDE/DE (where pDE and DE denote the pressure and density of DE, respectively), is one of the most important quantity used to describe the features of DE models. If we restrict ourselves to four-dimensional Einsteins gravity, almost all DE models can be classified according to the behavior of the EoS parameter as follows [38]: (i) Cosmological constant: w = 1; (ii) Quintessence: wQ 1; (iii) Phantom: wP 1 and (iv) Quintom: its EoS is able to evolve across the cosmological constant boundary. Scalar field models of dark energy are among the most promising and best elaborated ones to match observations of the accelerated expansion of the Universe. The phantom-like behavior of wDE may appear from BransDicke (BD) scalartensor gravity, from non-standard (negative) potentials, from the non-minimal coupling of a scalar Lagrangian with gravity, (...truncated)


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Surajit Chattopadhyay, Antonio Pasqua. New holographic reconstruction of scalar-field dark-energy models in the framework of chameleon Brans–Dicke cosmology, The European Physical Journal C, 2014, pp. 3080, Volume 74, Issue 9, DOI: 10.1140/epjc/s10052-014-3080-3