Ghost Dark Energy with Sign-changeable Interaction Term

Zadeh, M. Abdollahi; Sheykhi, Ahmad; Moradpour, H.

doi:10.1007/s10773-017-3513-5

Cited by 8 publications

(5 citation statements)

References 111 publications

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“…Observations also admit a sign-changeable interaction between the cosmos sectors [26][27][28]. Such interaction usually admits the cosmological models to experience a phantom phase [29].…”

Section: Introductionmentioning

confidence: 99%

Tsallis holographic dark energy in the Brans–Dicke cosmology

et al. 2018

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Using the Tsallis generalized entropy, holographic hypothesis and also considering the Hubble horizon as the IR cutoff, we build a holographic model for dark energy and study its cosmological consequences in the Brans-Dicke framework. At first, we focus on a non-interacting universe, and thereinafter, we study the results of considering a sign-changeable interaction between the dark sectors of the cosmos. Our investigations show that, compared with the flat case, the power and freedom of the model in describing the cosmic evolution is significantly increased in the presence of the curvature. The stability analysis also indicates that, independent of the universe curvature, both the interacting and non-interacting cases are classically unstable. In fact, both the classical stability criterion and an acceptable behavior for the cosmos quantities, including the deceleration and density parameters as well as the equation of state, are not simultaneously obtainable.

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“…Observations also admit a sign-changeable interaction between the cosmos sectors [26][27][28]. Such interaction usually admits the cosmological models to experience a phantom phase [29].…”

Section: Introductionmentioning

confidence: 99%

Tsallis holographic dark energy in the Brans–Dicke cosmology

et al. 2018

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“…This finding inspired the study of possible sign-switching interactions, instead of the classical monotonically decreasing or increasing parameterizations. We have for example: in [129] the parameterization Q(a) = 3b(a)H 0 ρ 0 was first proposed, with b(a) = b 0 a+b e (1−a) being the sign-switching part; in [130] the model Q = 3Hσ(ρ DE − αρ DM ) (α being a positive constant of order unity) also presents a switching interaction; in [131] the named Ghost dark energy is used in tandem with an interaction kernel Q = 3βHq(ρ DE + ρ DM ) where its sign is able to change since it is a function of the deceleration parameter q; and in [132] a bunch of variations of Q(a) = 3b(a)H(a)ρ i are studied. The general consensus reached by the majority of these models is that, if a transition were to happen, it should be around the time when the accelerated expansion of the Universe began (z ∼ 0.5).…”

Section: Introductionmentioning

confidence: 99%

Model-independent reconstruction of the interacting dark energy kernel: Binned and Gaussian process

Escamilla,

Akarsu,

Di Valentino

et al. 2023

J. Cosmol. Astropart. Phys.

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The cosmological dark sector remains an enigma, offering numerous possibilities for exploration. One particularly intriguing option is the (non-minimal) interaction scenario between dark matter and dark energy. In this paper, to investigate this scenario, we have implemented Binned and Gaussian model-independent reconstructions for the interaction kernel alongside the equation of state; while using data from BAOs, Pantheon+ and Cosmic Chronometers. In addition to the reconstruction process, we conducted a model selection to analyze how our methodology performed against the standard ΛCDM model. The results revealed a slight indication, of at least 1σ confidence level, for some oscillatory dynamics in the interaction kernel and, as a by-product, also in the DE and DM. A consequence of this outcome is the possibility of a sign change in the direction of the energy transfer between DE and DM and a possible transition from a negative DE energy density in early-times to a positive one at late-times. While our reconstructions provided a better fit to the data compared to the standard model, the Bayesian Evidence showed an intrinsic penalization due to the extra degrees of freedom. Nevertheless these reconstructions could be used as a basis for other physical models with lower complexity but similar behavior.

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Section: Introductionmentioning

confidence: 99%

“…On the other hand, observations admit a mutual interaction between DE and DM [75][76][77][78][79][80][81][82][83][84][85][86][87], and the CM B + BAO + SN + H 0 data suggests that the sign of mutual interaction has probably been changed during the cosmic evolution in the 0.45 ≤ z ≤ 0.9 interval [75]. This result motivates physicists to consider sign-changeable interactions, including the deceleration parameter [76][77][78][79][80][81][82][83][84][85][86][87]. Although the FLRW metric is a powerful tool in modeling the universe, and is in accordance with the cosmological principle [8], it does not compatible with the early universe anisotropy, and also the anisotropy of the cosmos in scales smaller than 100-Mpc and also [8].…”

Section: Introductionmentioning

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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Ghost Dark Energy with Sign-changeable Interaction Term

Cited by 8 publications

References 111 publications

Tsallis holographic dark energy in the Brans–Dicke cosmology

Tsallis holographic dark energy in the Brans–Dicke cosmology

Model-independent reconstruction of the interacting dark energy kernel: Binned and Gaussian process

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

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