Brans-Dicke理论中的全息暗能量
Holographic Dark Energy in Brans-Dicke Theory
摘要：
本文考虑Brans-Dicke理论中的全息暗能量模型，用$ρ_{h}=3c^2 Φ(t)L^{-2}$代替全息暗能量密度$ρ_Λ =3c^2 M^{2}_{pl} L^{-2}$。这里，$Φ(t)=\frac{1}{8πG}$是时间变量牛顿常数。通过这一替换，发现当哈勃视界作为红外截止时，宇宙不会加速膨胀。当采用事件视界作为红外截止时，得到了加速膨胀宇宙。在这种情况下，全息暗能量$w_h$的状态方程采用修改后的形式$w_h=-{1/3}(1+α+\frac{2}{c}\sqrt{Ω_{h}})$。在极限$α\to 0$中，“标准”全息暗能量被恢复。在全息暗能量占主导地位的时期，幂律和deSitter时空解。
英文摘要：
In this paper, the holographic dark energy model is considered in Brans-Dicke theory where the holographic dark energy density $ρ_Λ =3c^2 M^{2}_{pl} L^{-2}$ is replaced with $ρ_{h}=3c^2 Φ(t)L^{-2}$. Here $Φ(t)=\frac{1}{8πG}$ is a time variable Newton constant. With this replacement, it is found that no accelerated expansion universe will be achieved when the Hubble horizon is taken as the role of IR cut-off. When the event horizon is adopted as the IR cut-off, an accelerated expansion universe is obtained. In this case, the equation of state of holographic dark energy $w_h$ takes a modified form $w_h=-{1/3}(1+α+\frac{2}{c}\sqrt{Ω_{h}})$. In the limit $α\to 0$, the 'standard' holographic dark energy is recovered. In the holographic dark energy dominated epoch, power-law and de Sitter time-space solutions are obtained.
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