论文标题
DGP Braneworld宇宙学中的Tsallis年龄段的黑暗能量
Interacting Tsallis agegraphic dark energy in DGP Braneworld Cosmology
论文作者
论文摘要
本文的目的是研究DGP Brane-World场景中暗能和深色物质之间的相互作用项的Tsallis年龄段暗能。为此，我们假设一些初始条件以获得深色能量密度，减速，深色能量EOS和总EOS参数。然后，我们分析了状态基参数，$ω'{} _ {de}-Ω__{de} $图和模型的经典稳定性功能。结果表明，减速参数提供了从减速到加速相的相变。 $ω_{de} $图显示了幻影行为，而$ω__{tot} $在宇宙演变过程中表现出典型和幻影。遵循图表，状态基式分析显示了过去和现在模型的精髓行为。但是，在接下来的时代，它倾向于$λcdm$。 $ω'{} _ {de}-Ω__{de} $ plot指示解冻或冷冻区域，具体取决于$ b^{2} $，$δ$和$ m $的不同值和不同值的不同值。在声速的正方形上，我们看到该模型过去很稳定，当前时间是稳定或不稳定的，并且将来对于$ b^{2} $，$δ$和$ m $的选定值而言不稳定。为了测试模型，我们使用最近的哈勃数据。我们还采用Akaike信息标准（AIC）和贝叶斯信息标准（BIC）将模型与$λCDM$作为参考模型进行比较。此外，我们使用$ H-Z $图测试模型，并在将来看到一个转折点。 $ω_{TOT} $图的最佳拟合值的结果强调，宇宙在当前时间位于典型区域。它将进入幻影阶段，然后将来接近$λ$状态。但是，$ω__{de} $总是留在幻影区域。该模型在当前和进步时代是不稳定的。
The purpose of this paper is to study the Tsallis agegraphic dark energy with an interaction term between dark energy and dark matter in the DGP brane-world scenario. For this, we assume some initial conditions to obtain the dark energy density, deceleration, dark energy EoS, and total EoS parameters. Then, we analyze the statefinder parameters, $ω'{}_{DE}-ω_{DE}$ plots, and classical stability features of the model. The results state that the deceleration parameter provides the phase transition from decelerated to accelerated phase. The $ω_{DE}$ graphs show the phantom behavior, while the $ω_{tot}$ exhibits the quintessence and phantom during the evolution of the Universe. Following the graphs, the Statefinder analysis shows the quintessence behavior of the model for the past and present. However, it tends to the $ΛCDM$ in the following era. The $ω'{}_{DE}-ω_{DE}$ plot indicates the thawing or freezing area depending on the type of era and different values of $b^{2}$, $δ$, and $m$. By the square of the sound speed, we see the model is stable in the past, stable or unstable at the current time, and unstable in the future for selected values of $b^{2}$, $δ$, and $m$. To test the model, we use the recent Hubble data. We also employ Akaike Information Criterion (AIC) and Bayesian Information Criterion (BIC) to compare the model with the $ΛCDM$ as the reference model. In addition, we test the model using the $H-z$ plot, and we see a turning point in the future time. The results from the best fit values for the $ω_{tot}$ plot emphasize that the Universe is in the quintessence region in the current time. It will enter the phantom phase, and then it will approach the $Λ$ state in the future. But, the $ω_{DE}$ always stays on the phantom region. The model is unstable in the present and progressive era.
