论文标题
修改的$ f（q）$ - 重力
Quintessence Behaviour of an Anisotropic Bulk Viscous Cosmological Model in Modified $f(Q)$-Gravity
论文作者
论文摘要
在本文中，我们讨论了调查的结果。我们考虑了（LRS）Bianchi I型时空宇宙的各向异性粘性宇宙学模型，该宇宙充满了$ f（q）$重力下的粘性液体。我们已经研究了修改后的$ f（q）$重力，其中二次形式$ f（q）=αq^{2}+β$，其中$ q $称为非内方标量表，$α$，$β$是正常数。我们通过考虑粘度系数$ξ（t）=ξ_{0} h $并获得比例因子$ a（t）= 2〜sinh \ left（\ frac {m+ 2}），我们获得了修改的爱因斯坦字段方程 {6}\sqrt{\frac{ξ_{0}}{α(2m+1)}}t\right)$.We applied the observational constraint on the apparent magnitude $m(z)$ using the $χ^{2}$ test formula with observational data set like JLA or Union 2.1 compilation and obtained the best approximate values of the model parameters $ {m，α，h_ {0}ξ_{0}} $。我们已经分析了我们的模型，并发现了一个过境相的各向异性加速宇宙。我们还检查了状态（EOS）参数$ω_{v} $的大量粘度方程，并获得了其当前值为$ω__{V} <-1/3 $，该值显示了深色能量主导模型，宇宙学常数，幻影，幻影，幻象和超级平tom的深色能量模型，并倾向于$λ$ cdm $ cdm $ cdm $ cdm $ cdm $Ω我们还将宇宙的当前年龄估计为$ t_ {0} \ oft13.6 $ grys，并用$（s，r）\ to（0,1）$分析了statefinder参数为$ t \ to \ infty $。
In this article, we have discussed the results of our investigation. We consider an anisotropic viscous cosmological model of (LRS) Bianchi type I spacetime universe filled with a viscous fluid under $f(Q)$ gravity. We have studied the modified $f(Q)$ gravity with quadratic form $f(Q)=αQ^{2}+β$, where $Q$ is called as a non-metricity scalar and $α$, $β$ are positive constants. We obtain the modified Einstein field equation by considering the viscosity coefficient $ξ(t)=ξ_{0}H$ and obtained the scale factor $a(t)=2~sinh\left (\frac{m+ 2} {6}\sqrt{\frac{ξ_{0}}{α(2m+1)}}t\right)$.We applied the observational constraint on the apparent magnitude $m(z)$ using the $χ^{2}$ test formula with observational data set like JLA or Union 2.1 compilation and obtained the best approximate values of the model parameters ${ m,α, H_{0} ξ_{0}}$. We have analyzed our model and found a transit phase quintessence anisotropic accelerating universe. We also examined the bulk viscosity equation of state (EoS) parameter $ω_{v}$ and obtained its current value as $ω_{v}<-1/3$, which shows the dark energy dominant model, cosmological constant, phantom, and super-phantom dark energy models, and tends to the $Λ$CDM value ($ω_{v}=-1$) in the late time. We also estimate the current age of the universe as $t_{0}\approx13.6$ Grys and analyze the Statefinder parameters with $(s,r)\to(0,1)$ as $t \to \infty$.
