Constraining Parameters for the Accelerating Models in Symmetric Teleparallel Gravity

A., Narawade, S.; Shekh, S. H.; Mishra, B.; Khyllep, Wompherdeiki; Dutta, Jibitesh

doi:10.2139/ssrn.4374178

Cited by 4 publications

(4 citation statements)

References 55 publications

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“…which is dubbed as Invf (Q) model [10,14,36] since additional term is the inverse of Q. Here Q 0 = Q(z = 0) for the current universe.…”

Section: Models and Resultsmentioning

confidence: 99%

Cosmological constraints in covariant f(Q) gravity with different connections

Shi

2023

Eur. Phys. J. C

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Recently it has been shown that the cosmological dynamics of covariant f(Q) gravity depend on different affine connections. In this paper, two specific f(Q) models are investigated with SNe+CC+BAO+QSO observational data, and the spatial curvature of the universe is studied in covariant f(Q) gravity. It is found that the parameters $${\mathcal {X}}_0$$ X 0 and $${\mathcal {X}}'_0$$ X 0 ′ characterizing affine connections significantly affect the behavior of the effective equation of state $$w_Q$$ w Q and may drive it across the phantom divide line. These results imply some inertial effects of the universe change the cosmic dynamics. However based on the Bayesian evidence, the zero inertial effect is more favored in the flat universe. Moreover, a closed universe is favored not only in the $$\Lambda $$ Λ CDM model but also in covariant f(Q) gravity. The f(Q) models have less support evidence than the $$\Lambda $$ Λ CDM model in the non-flat universe.

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“…which is dubbed as Invf (Q) model [10,14,36] since additional term is the inverse of Q. Here Q 0 = Q(z = 0) for the current universe.…”

Section: Models and Resultsmentioning

confidence: 99%

Cosmological constraints in covariant f(Q) gravity with different connections

Shi

2023

Eur. Phys. J. C

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“…In order to achieve that we perform a dynamicalsystem analysis [89,90], which allows one to extract the global features of a cosmological scenario independently of the specific initial conditions [91][92][93][94][95][96][97]. Note that the dynamical-system analysis for f (Q) gravity has been performed in the literature [98][99][100][101][102], however it remains in the flat FLRW case, while as we will see in the following the inclusion of spatial curvature leads to novel qualitative features.…”

Section: Cosmological Behaviormentioning

confidence: 99%

Cosmology of f(Q) gravity in non-flat Universe

Shabani,

De,

Loo

et al. 2024

Eur. Phys. J. C

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We investigate the cosmological implications of f(Q) gravity, which is a modified theory of gravity based on non-metricity, in non-flat geometry. We perform a detailed dynamical-system analysis keeping the f(Q) function completely arbitrary. As we show, the cosmological scenario admits a dark-matter dominated point, as well as a dark-energy dominated de Sitter solution which can attract the Universe at late times. However, the main result of the present work is that there are additional critical points which exist solely due to curvature. In particular, we find that there are curvature-dominated accelerating points which are unstable and thus can describe the inflationary epoch. Additionally, there is a point in which the dark-matter and dark-energy density parameters are both between zero and one, and thus it can alleviate the coincidence problem. Finally, there is a saddle point which is completely dominated by curvature. In order to provide a specific example, we apply our general analysis to the power-law case, showing that we can obtain the thermal history of the Universe, in which the curvature density parameter may exhibit a peak at intermediate times. These features, alongside possible indications that non-zero curvature could alleviate the cosmological tensions, may serve as advantages for f(Q) gravity in non-flat geometry.

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“…and z tr = 0.65 +0.08 −0.07 in scalar field [67] and q 0 = −0.5422 +0.0718 −0.0826 and z tr = 0.65 +0. 19 −0.17 in f (Q, T) gravity [68] and q 0 = −0.423 and z tr = 0.665 in f (T) gravity. [69] Hence, our results are compatible with the current observable data.…”

Section: Behavior Of the Physical Parametersmentioning

confidence: 99%

Dynamical System Approach and Thermodynamical Perspective of Hořava‐Lifshitz Gravity

Samaddar,

Singh

2024

Fortschritte der Physik

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The authors have examined a Friedmann Robertson Walker cosmological model in Hořava‐Lifshitz gravity by using a dynamical system approach. A set of autonomous equations is derived and their solutions are calculated. The critical points from these equations and find the characteristics values with the analysis of the physical interpretation of the phase space for this system are assessed. Three stable critical points are found and the values of the physical parameters and the scale factor's expressions at each critical points are displayed in Tables 1, 2, and 3. A hybrid scale factor to develop the model, which results in a phase transition from deceleration to acceleration is used. The suitable values of the parameters are governed by applying the Monte Chain Monte Carlo method technique to the Hubble 46 and joint Hubble 46 and Baryon Acoustic Oscillations 15 datasets. In contrast to the negative behavior of pressure, the positive behavior of energy density and illustrate the Universe's acceleration epoch and the model is represented by the EoS parameter . The authors investigated that the energy conditions and their model violates the strong energy condition. Utilizing diagnostic test, it is found that the model represents phantom behavior. The thermodynamical perspective for the model is also examined. The model accurately explained the Universe's propagation history and fits well with contemporary cosmic data.

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Constraining Parameters for the Accelerating Models in Symmetric Teleparallel Gravity

Cited by 4 publications

References 55 publications

Cosmological constraints in covariant f(Q) gravity with different connections

Cosmological constraints in covariant f(Q) gravity with different connections

Cosmology of f(Q) gravity in non-flat Universe

Dynamical System Approach and Thermodynamical Perspective of Hořava‐Lifshitz Gravity

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