Consistency of nonlinear interacting ghost dark energy with recent observations

Ebrahimi, Esmaeil; Golchin, Hanif; Mehrabi, Ahmad; Movahed, M. Sadegh

doi:10.1142/s0218271817501243

Cited by 11 publications

(4 citation statements)

References 134 publications

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“…This model is a five-dimensional bulk with self-accelerating and normal characteristics. The self-accelerating characteristic of the DGP model is able to show the late-time acceleration [31][32][33][34][35][36][37][38][39]. But, this characteristic of the DGP model cannot satisfy the phantom divide crossing by itself.…”

Section: Introductionmentioning

confidence: 99%

Interacting Tsallis agegraphic dark energy in DGP Braneworld Cosmology

Mangoudehi

2022

Preprint

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The purpose of this paper is to study the Tsallis agegraphic dark energy with an interaction term between dark energy and dark matter in the DGP brane-world scenario. For this, we assume some initial conditions to obtain the dark energy density, deceleration, dark energy EoS, and total EoS parameters. Then, we analyze the statefinder parameters, ω DE − ω DE plots, and classical stability features of the model. The results state that the deceleration parameter provides the phase transition from decelerated to accelerated phase. The ω DE graphs show the phantom behavior, while the ω tot exhibits the quintessence and phantom during the evolution of the Universe.Following the graphs, the Statefinder analysis shows the quintessence behavior of the model for the past and present. However, it tends to the ΛCDM in the following era. The ω DE − ω DE plot indicates the thawing or freezing area depending on the type of era and different values of b 2 , δ, and m. By the square of the sound speed, we see the model is stable in the past, stable or unstable at the current time, and unstable in the future for selected values of b 2 , δ, and m. To test the model, we use the recent Hubble data. We also employ Akaike Information Criterion (AIC) and Bayesian Information Criterion (BIC) to compare the model with the ΛCDM as the reference model. In addition, we test the model using the H − z plot, and we see a turning point in the future time. The results from the best fit values for the ω tot plot emphasize that the Universe is in the quintessence region in the current time. It will enter the phantom phase, and then it will approach the Λ state in the future. But, the ω DE always stays on the phantom region. The model is unstable in the present and progressive era.

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Section: Introductionmentioning

confidence: 99%

Interacting Tsallis agegraphic dark energy in DGP Braneworld Cosmology

Mangoudehi

2022

Preprint

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“…Mamon et al [26] have considered dimensionless dark energy function to reconstruct the DE cosmological model. Ebrahimi et al [27] have established a non-linear interaction of dark energy and dark matter to construct ghost DE cosmological model. Several cosmological models have been constructed to address the cosmic acceleration problem using different space times and different matter fields [28][29][30][31].…”

Section: Introductionmentioning

confidence: 99%

Axially magnetized dark energy cosmological model

et al. 2019

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We investigate the behaviour of the skewness parameters for an anisotropic universe in the framework of General Relativity. Non interacting dark energy is considered in presence of electromagnetic field. A time varying deceleration parameter simulated by a hybrid scale factor is considered. The dynamics of the universe is investigated in presence and absence of magnetic field. The equation of state parameter of dark energy evolves within the range predicted by the observations. Magnetic field is observed to have a substantial effect on the cosmic dynamics and the skewness parameters. The models discussed here end in a big rip and become isotropic at finite time. PACS numbers:PACS number:04.50.kd.

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“…An attitude toward avoiding the coincidence problem also is the usage of interaction term as a nongravitational component between dark sectors [44][45][46][47][48][49](to mention a few). In addition, because of the degeneracy between dark sectors in the Einstein's gravity, it could be assumed that there is a non-gravitational coupling/interaction between them which can be non-linear [50][51][52][53][54][55][56]. These kinds of interaction term can be used for probing the dark energy related problems.…”

Section: Introductionmentioning

confidence: 99%

Scrutinizing Various Phenomenological Interactions In The Context Of Holographic Ricci Dark Energy Models

Sadri,

Khurshudyan,

Zeng

2019

Preprint

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In this paper, we examine two types of interacting holographic dark energy model using Pantheon supernova data, BAO BOSS DR12, CMB Planck 2015, fgas (gas mass fraction) and SZ/Xray (Sunyaev-Zeldovich effect and X-ray emission) data from galaxy clusters (GC). In particular, we considered the Holographic Ricci dark energy and Extended holographic Ricci dark energy models. During this analysis we considered seven type of phenomenological interaction terms (three linear and four non-linear)

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Consistency of nonlinear interacting ghost dark energy with recent observations

Cited by 11 publications

References 134 publications

Interacting Tsallis agegraphic dark energy in DGP Braneworld Cosmology

Interacting Tsallis agegraphic dark energy in DGP Braneworld Cosmology

Axially magnetized dark energy cosmological model

Scrutinizing Various Phenomenological Interactions In The Context Of Holographic Ricci Dark Energy Models

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