f(T) theories from holographic dark energy models within Bianchi type I universe

Fayaz, V.; Hossienkhani, H.; Pasqua, Antonio; Amirabadi, M.; Ganji, Masoud

doi:10.1140/epjp/i2015-15028-2

Cited by 28 publications

(15 citation statements)

References 90 publications

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“…It is important to note that when b 2 = 0, the interacting DE becomes inevitable and Eq. ( 49) reduces to its respective expression in new ADE in general relativity [70]. In the case of (b 2 = 0), the present accelerated expansion of our universe can be derived only if n > 1 [29].…”

Section: Correspondence Between the Interacting New Agegraphic De And...mentioning

confidence: 92%

Effect of anisotropy on the generalized Chaplygin gas scalar field and its interaction with other dark energy models

2017

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In this work, we establish a correspondence between the interacting holographic, new agegraphic dark energy and generalized Chaplygin gas model in Bianchi type I universe. In continue, we reconstruct the potential of the scalar field which describes the generalized Chaplygin cosmology. Cosmological solutions are obtained when the kinetic energy of the phantom field is order of the anisotropy and dominates over the potential energy of the field. We investigate observational constraints on the generalized Chaplygin gas, holographic and new agegraphic dark energy models as the unification of dark matter and dark energy, by using the latest observational data. To do this we focus on observational determinations of the expansion history H(z). It is shown that the HDE model is better than the NADE and generalized Chaplygin gas models in an anisotropic universe. Then, we calculate the evolution of density perturbations in the linear regime for three models of dark energy and compare the results ΛCDM model. Finally, the analysis shows that the increase in anisotropy leads to more correspondence between the dark energy scalar field model and observational data.

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Section: Correspondence Between the Interacting New Agegraphic De And...mentioning

confidence: 92%

Effect of anisotropy on the generalized Chaplygin gas scalar field and its interaction with other dark energy models

2017

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“…where ρ D and ω D (≡ pD ρD ) represent the energy density and EoS parameter of dark energy, respectively, and p D denotes the DE pressure. In this manner, the corresponding Friedmann equations (the BI equations) take the form [109][110][111]…”

Section: General Frameworkmentioning

confidence: 99%

Effects of anisotropy on the sign-changeable interacting Tsallis holographic dark energy

et al. 2019

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A spatially homogeneous and anisotropic Bianchi type I universe is considered while it is filled by pressureless dark matter (DM) and Tsallis holographic dark energy (DE) interacting with each other throughout a sign-changeable mutual interaction. Various infra-red (IR) cutoffs are studied, and it has been obtained that while the current universe can classically be stable for some cases, all models display classical instability by themselves at the future (z → −1). Moreover, we find out that some models can cross the phantom line. In order to have a more comprehensive study, the statefinder diagnostic and the ωD − ω ′ D plane are also investigated showing that the model parameters significantly affect the evolution trajectories in the r − s and ωD − ω ′ D planes. *

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“…Oliveros and Acero [15] studied this NHDE approach in the vicinity of the FRW metric with a non-linear interaction between DE and DM, and discussed the portrait of the equation of state (EoS) parameter ω D , on the ω D −ω D plane, as well as its behavior with the aid of the Om-diagnostic tool. Fayaz et al [16] investigated HDE model in a Bianchi Type I with (BI) universe within the context of the generalized teleparallel theory and found phantom/quintessence regions of the universe. Sadri and Vakili [17] studied the NHDE approach in BD theory using a FRW universe model with logarithmic scalar field, and analyzed the EoS/deceleration parameter, statefinder and Om-diagnostic tool for both non-interacting/interacting case.…”

Section: Introductionmentioning

confidence: 99%

New Holographic Dark Energy Model in Brans-Dicke Theory

2018

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Abstract:We study the cosmic evolution of the Bianchi type I universe by using new holographic dark energy model in the context of the Brans-Dicke theory for both non-interacting and interacting cases between dark energy and dark matter. We evaluate the equation of state for dark energy ω D and draw the ω D −ω D plane, where the dot denotes the time derivative. It is found that a stage in which the cosmic expansion is accelerating can be realized in both cases. In addition, we investigate the stability of the model by analyzing the sound speed. As a result, it is demonstrated that for both cases, the behavior of the sound speed becomes unstable. Furthermore, with the Om-diagnostic tool, it is shown that the quintessence region of the universe can exist.

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f(T) theories from holographic dark energy models within Bianchi type I universe

Cited by 28 publications

References 90 publications

Effect of anisotropy on the generalized Chaplygin gas scalar field and its interaction with other dark energy models

Effect of anisotropy on the generalized Chaplygin gas scalar field and its interaction with other dark energy models

Effects of anisotropy on the sign-changeable interacting Tsallis holographic dark energy

New Holographic Dark Energy Model in Brans-Dicke Theory

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