How Different Connections in Flat FLRW Geometry Impact Energy Conditions in f(Q)$f(Q)$ Theory?

Ganesh, Subramaniam; De, Avik; Loo, Tee‐How; Goh, Yong Kheng

doi:10.1002/prop.202300038

Cited by 9 publications

(1 citation statement)

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“…Particular forms of the f (Q) function have been demonstrated to alleviate the σ8 tension [5], whereas others enable a more accurate representation of cosmological data [6][7][8]. Recently, some interesting cosmological implications of the f (Q) gravity in the different context have been appeared, for instance, Black hole physics [9,10], Neutrino physics [11], Quantum cosmology [12,13], Bouncing Cosmology [14], Inflation [15], Phantom cosmology [16], Astrophysical objects [17,18], Cosmological perturbations [19], BBN constraints [20], and many others [21][22][23][24][25].…”

Section: Introductionmentioning

confidence: 99%

Dynamical system analysis of scalar field cosmology in coincident f(Q) gravity

Ghosh,

Solanki,

Sahoo

2024

Phys. Scr.

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In this article, we investigate scalar field cosmology in the coincident $f(Q)$ gravity formalism. We calculate the motion equations of $f(Q)$ gravity under the flat Friedmann-Lema\^{i}tre-Robertson-Walker background in the presence of a scalar field. We consider a non-linear $f(Q)$ model, particularly $f(Q)=-Q+\alpha Q^n$, which is nothing but a polynomial correction to the STEGR case. Further, we assumed two well-known specific forms of the potential function, specifically the exponential from $V(\phi)= V_0 e^{-\beta \phi}$ and the power-law form $V(\phi)= V_0\phi^{-k}$. We employ some phase-space variables and transform the cosmological field equations into an autonomous system. We calculate the critical points of the corresponding autonomous systems and examine their stability behaviors. We discuss the physical significance corresponding to the exponential case for parameter values $n=2$ and $n=-1$ with $\beta=1$, and $n=-1$ with $\beta=\sqrt{3}$. Moreover, we discuss the same corresponding to the power-law case for the parameter value $n=-2$ and $k=0.16$. We also analyze the behavior of corresponding cosmological parameters such as scalar field and dark energy density, deceleration, and the effective equation of state parameter. Corresponding to the exponential case, we find that the results obtained for the parameter constraints in Case III is better among all three cases, and that represents the evolution of the universe from a decelerated stiff era to an accelerated de-Sitter era via matter-dominated epoch. Further, in the power-law case, we find that all trajectories exhibit identical behavior, representing the evolution of the universe from a decelerated stiff era to an accelerated de-Sitter era. Lastly, we conclude that the exponential case shows better evolution as compared to the power-law case.

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