Lambert函数分布的$f\left( Q\right)$对称平行引力场中的Barrow全息暗能量模型
Barrow holographic dark energy models in $f\left( Q\right)$ symmetric teleparallel gravity with Lambert function distribution
摘要：
在$% f\left( Q\right) $对称遥平行引力理论框架下，研究了Barrow最近提出的各向异性Bianchi I型宇宙中的Barrow全息暗能量（红外截止为哈勃视界）（Physics Letters B 808（2020）：135643），其中非度规标量$% f\left( Q\right) $负责引力相互作用.我们考虑两种情况：无压暗物质和巴罗全息暗能量的相互作用和非相互作用模型通过求解$f\left( Q\right) $对称远程平行场方程。为了求出场方程的精确解，我们假设时间-红移关系服从朗伯函数分布$t\left( z\right) =\frac{mt_{0}}{l}g\left( z\right) $，其中$g\left( z\right) =LambertW\left[ \frac{l}{m}e^{\frac{l-\ln \left( 1+z\right) }{m}}\right] $，$m$和$l$为非负常数，$t_{0}$代表宇宙的年龄.此外，我们讨论了几个宇宙学参数，如能量密度，状态方程（EoS）和偏态参数，平方声速，和$(ω_{B}-ω_{B}^{^{\prime }})$平面。最后，我们得到了朗伯函数分布的减速参数（DP）值$q_{(z=0)}=-0.45$和$q_{(z=-1)}=-1$，它们与最近的观测数据相一致，即DP随宇宙时间从初始减速到后期加速演化。
英文摘要：
The paper presents Barrow holographic dark energy (infrared cut-off is the Hubble horizon) suggested by Barrow recently (Physics Letters B 808 (2020): 135643) in an anisotropic Bianchi type-I Universe within the framework of $% f\left( Q\right) $ symmetric teleparallel gravity, where the non-metricity scalar $Q$ is responsible for the gravitational interaction. We consider two cases: Interacting and non-interacting models of pressureless dark matter and Barrow holographic dark energy by solving $f\left( Q\right) $ symmetric teleparallel field equations. To find the exact solutions of the field equations, we assume that the time-redshift relation follows a Lambert function distribution as $t\left( z\right) =\frac{mt_{0}}{l}g\left( z\right) $, where $g\left( z\right) =LambertW\left[ \frac{l}{m}e^{\frac{l-\ln \left( 1+z\right) }{m}}\right] $, $m$ and $l$ are non-negative constants and $t_{0}$ represents the age of the Universe. Moreover, we discuss several cosmological parameters such as energy density, equation of state (EoS) and skewness parameters, squared sound speed, and $(ω_{B}-ω_{B}^{^{\prime }})$ plane. Finally, we found the values of the deceleration parameter (DP) for the Lambert function distribution as $q_{(z=0)}=-0.45$ and $q_{(z=-1)}=-1$ which are consistent with recent observational data, i.e. DP evolves with cosmic time from initial deceleration to late-time acceleration.
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