Testing the Interacting Dark Energy Model with Cosmic Microwave Background Anisotropy and Observational Hubble Data

Yang, Weiqiang; Xu, Lixin; Li, Hang; Wu, Yabo; Lu, Jianbo

doi:10.3390/e19070327

Cited by 10 publications

(2 citation statements)

References 73 publications

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“…x y q ω de ω eff Ω de /Ω dm Type of stability C.P. 3 considered parametrization of the dark side of the Universe is valid for lower redshifts, therefore it is reasonable to expect that the reconstructed low redshift behavior of the parameters is correct and correspond to the recent Universe. We should highlight that this is correct for the parameters reconstructed using the reconstructed Hubble data, and not the Hubble data itself.…”

Section: The Models Phase Space Analysis and Gp Processesmentioning

confidence: 99%

Cosmological singularities in interacting dark energy models with an ω(q) parametrization

Elizalde

Khurshudyan

Nojiri

2019

Int. J. Mod. Phys. D

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Future singularities arising in a family of models for the expanding Universe, characterized by sharing a convenient parametrization of the energy budget in terms of the deceleration parameter, are classified. Finite-time future singularities are known to appear in many cosmological scenarios, in particular, in the presence of viscosity or non-gravitational interactions, the last being known to be able to suppress or just change in some cases the type of the cosmological singularity. Here, a family of models with a parametrization of the energy budget in terms of the deceleration parameter are studied in the light of Gaussian processes using reconstructed data from 40-value H(z) datasets. Eventually, the form of the possible non-gravitational interaction between dark energy and dark matter is constructed from these smoothed H(z) data. Using phase space analysis, it is shown that a non-interacting model with dark energy ω de = ω0 + ω1q (q being the deceleration parameter) may evolve, after starting from a matter dominated unstable state, into a de Sitter Universe (the solution being in fact a stable node). Moreover, for a model with interaction term Q = 3Hbρ dm (b is a parameter and H the Hubble constant) three stable critical points are obtained, what may have important astrophysical implications. In addition, part of the paper is devoted to a general discussion of the finite-time future singularities obtained from direct numerical integration of the field equations, since they appear in many cosmological scenarios and could be useful for future extended studies of the models here introduced. Numerical solutions for the new models, produce finite-time future singularities of Type I or Type III, or an ω-singularity, provided general relativity describes the background dynamics. 95.36.+x, 98.80.Jk, 98.80.Cq

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Section: The Models Phase Space Analysis and Gp Processesmentioning

confidence: 99%

Cosmological singularities in interacting dark energy models with an ω(q) parametrization

Elizalde

Khurshudyan

Nojiri

2019

Int. J. Mod. Phys. D

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“…Unlike the well behaved non-interacting models with constant w (given a barotropic equation state, where w is the proportionality parameter), an interacting model can manifest instabilities in the perturbations of the dark-sector at early times giving rise to new phenomena. Interacting dark-sector models have, for example, been studied in [18][19][20][21][22][23][24][25] This article is arranged as follows; section(2) discusses multi-fluid and the convective variational formalism. Section (3) discusses DE and DM , while section (4) discusses the Lagrangian formulation involving interacting dark-sector and coresponding equations of motion.…”

Section: Introductionmentioning

confidence: 99%

Multi-fluid theory and cosmology: A convective variational approach to interacting dark-sector

Osano

Oreta

2019

Int. J. Mod. Phys. D

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This article examines the foundation of the recently developed relativistic variational formalism [1]. Our work is heavily based on [2,27] which extends this approach to the multi-fluid theory and examines its utility in astrophysics and cosmology. Unlike the extension to the formalism mentioned above, that looks at the general interaction between different types of matter, we use the formalism to examine the interaction involving, ordinary matter, dark matter (DM ) and dark energy (DE). We focus on an entrainment phenomena involving the dark-sector constituents.1.

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Modified f(Q)-gravity string cosmological models with observational constraints

Maurya,

Singh

2024

Astronomy and Computing

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Testing the Interacting Dark Energy Model with Cosmic Microwave Background Anisotropy and Observational Hubble Data

Cited by 10 publications

References 73 publications

Cosmological singularities in interacting dark energy models with an ω(q) parametrization

Cosmological singularities in interacting dark energy models with an ω(q) parametrization

Multi-fluid theory and cosmology: A convective variational approach to interacting dark-sector

Modified f(Q)-gravity string cosmological models with observational constraints

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