Cosmological constraints of interacting phantom dark energy models

Bouali, Amine; Albarran, Imanol; Bouhmadi-López, Mariam; Errahmani, Ahmed; Ouali, Taoufik

doi:10.1016/j.dark.2021.100907

Cited by 16 publications

(5 citation statements)

References 88 publications

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“…For generalizations, one could also consider interactions between the two dark energy components with dark matter and/or dark radiation in a more complicated model (a quintom model was considered in [90], with the phantom component interacting with dark matter, but not with the quintessence sector; see also [91]). Another possibility is to consider other forms of interaction terms in place of ±γρ Λ 1 ρ Λ 2 ; see, for example, [92] and the references therein for the case of DM-DE interaction. Most importantly, more realistic models need to go beyond the assumption that the Hubble parameter is slowly varying when setting up the Lotka-Volterra equations.…”

Section: Discussion: Sign Switching Dark Energy and Naturalnessmentioning

confidence: 99%

An Effective Sign Switching Dark Energy: Lotka–Volterra Model of Two Interacting Fluids

Ong

2023

Universe

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One of the recent attempts to address the Hubble and S8 tensions is to consider that the Universe started out not as a de Sitter-like spacetime, but rather anti-de Sitter-like. That is, the Universe underwent an “AdS-to-dS” transition at some point. We study the possibility that there are two dark energy fluids, one of which gave rise to the anti-de Sitter-like early Universe. The interaction is modeled by the Lotka–Volterra equations commonly used in population biology. We consider “competition” models that are further classified as “unfair competition” and “fair competition”. The former involves a quintessence in competition with a phantom, and the second involves two phantom fluids. Surprisingly, even in the latter scenario it is possible for the overall dark energy to cross the phantom divide. The latter model also allows a constant w “AdS-to-dS” transition, thus evading the theorem that such a dark energy must possess a singular equation of state. We also consider a “conversion” model in which a phantom fluid still manages to achieve “AdS-to-dS” transition even if it is being converted into a negative energy density quintessence. In these models, the energy density of the late time effective dark energy is related to the coefficient of the quadratic self-interaction term of the fluids, which is analogous to the resource capacity in population biology.

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Section: Discussion: Sign Switching Dark Energy and Naturalnessmentioning

confidence: 99%

An Effective Sign Switching Dark Energy: Lotka–Volterra Model of Two Interacting Fluids

Ong

2023

Universe

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“…For radiation, p r = 1 3 𝜌 r , so we obtain 𝜌 r = 𝜌 r0 a −4 through Equation (6). Since the DM follows negligible pressure, i.e., p m = 0, thereby we get 𝜌 m = 𝜌 m0 a −3 using Equation (7).…”

Section: Basic Equations Of Frw Modelmentioning

confidence: 99%

“…Among them, the ΛCDM model is widely accepted as supposedly it 'best accommodates' the observations but also comes up with some ambiguities like fine-tuning and coincidence problems, etc. [3][4][5] To overcome these drawbacks, several alternatives for DE models like a quintessence, phantom, [6,7] k-essence, and Chaplygin gas etc. [8] have been presented in order to effectively address some valid queries about the cosmos and discuss abundant aspects of the exotic energy.…”

Section: Introductionmentioning

confidence: 99%

Observational Constraining Study of New Deceleration Parameters in FRW Universe

Bouali

Chaudhary

Mumtaz

et al. 2023

Fortschritte der Physik

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In the current paper, a dark energy (DE) model reconstructed from the well‐motivated deceleration parameter (DP) is analyzed. A flat FRW Universe filled with radiation, dark matter (DM), and dark energy fluids is considered. The free parameters are constrained using measurements from Supernovae, Hubble, Gamma Ray Bursts, Quasars, and Baryon acoustic Oscillations. The model under study is found to be very supported by observation with respect to ΛCDM since . Besides, a cosmographic analysis is performed showing that the reconstructed model behaves similarly as ΛCDM does. Finally, a diagnostic analysis is performed reporting that the studied model behaves quintessence type at a late time.

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“…Indeed, its Hubble rate H diverges while its derivative Ḣ remains constant. This abrupt event has been well studied in [48][49][50] and dubbed as Little Sibling of the Big Rip since it smooths the big rip singularity in the future.…”

Section: Introductionmentioning

confidence: 99%

Smoothing the $H_0$ tension with a dynamical dark energy model

Dahmani¹,

Bouali²,

Bojaddaini³

et al. 2023

Preprint

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The discrepancy between Planck data and direct measurements of the current expansion rate H0 and the matter fluctuation amplitude S8 has become one of the most intriguing puzzles in cosmology nowadays. The H0 tension has reached 4.2σ in the context of standard cosmology i.e ΛCDM. Therefore, explanations to this issue are mandatory to unveil its secrets. Despite its success, ΛCDM is unable to give a satisfying explanation to the tension problem. Unless some systematic errors might be hidden in the observable measurements, physics beyond the standard model of cosmology must be advocated. In this perspective, we study a phantom dynamical dark energy model as an alternative to ΛCDM in order to explain the aforementioned issues. This phantom model is characterised by one extra parameter, Ω pdde , compared to ΛCDM. We obtain a strong positive correlation between H0 and Ω pdde , for all data combinations. Using Planck measurements together with BAO and Pantheon, we find that the H0 and the S8 tensions are 3σ and 2.6σ, respectively. By introducing a prior on the absolute magnitude, MB, of the SN Ia, the H0 tension decreases to 2.27σ with H0 = 69.76 +0.75 −0.82 km s −1 Mpc −1 and the S8 tension reaches the value 2.37σ with S8 = 0.8269 +0.011 −0.012 .

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Cosmological constraints of interacting phantom dark energy models

Cited by 16 publications

References 88 publications

An Effective Sign Switching Dark Energy: Lotka–Volterra Model of Two Interacting Fluids

An Effective Sign Switching Dark Energy: Lotka–Volterra Model of Two Interacting Fluids

Observational Constraining Study of New Deceleration Parameters in FRW Universe

Smoothing the $H_0$ tension with a dynamical dark energy model

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