全息椭球宇宙学中的哈勃IR截止
The Hubble IR cutoff in holographic ellipsoidal cosmologies
摘要：
众所周知，对于空间平坦的FRW宇宙学，全息暗能量不利于哈勃参数作为红外截止的候选者。为了克服这个问题，我们探索了在全息椭球宇宙学模型中使用这种截断，并导出了由这种全息能量密度引起的一般椭球度规。尽管这种截断存在于均匀和各向同性宇宙中的缺点，但基于这一通用度量，我们开发了一个合适的椭球全息宇宙学模型，充满了暗物质和暗能量分量。在后期阶段，宇宙演化是由全息各向异性暗能量与正压状态方程。宇宙学以加速的方式向各个方向扩展。由于这里给出的椭球宇宙学不是渐近FRW，在大宇宙尺度上宇宙的均匀性和各向同性的偏离在所有宇宙演化过程中保持不变。这一特征使得研究的全息椭球宇宙学可以由状态方程$ω=p/ρ$来控制，其范围属于精华甚至幻影物质。
英文摘要：
It is well known that for spatially flat FRW cosmologies, the holographic dark energy disfavours the Hubble parameter as a candidate for the IR cutoff. For overcoming this problem, we explore the use of this cutoff in holographic ellipsoidal cosmological models, and derive the general ellipsoidal metric induced by a such holographic energy density. Despite the drawbacks that this cutoff presents in homogeneous and isotropic universes, based on this general metric, we developed a suitable ellipsoidal holographic cosmological model, filled with a dark matter and a dark energy components. At late time stages, the cosmic evolution is dominated by a holographic anisotropic dark energy with barotropic equations of state. The cosmologies expand in all directions in accelerated manner. Since the ellipsoidal cosmologies given here are not asymptotically FRW, the deviation from homogeneity and isotropy of the universe on large cosmological scales remains constant during all cosmic evolution. This feature allows studied holographic ellipsoidal cosmologies to be ruled by an equation of state $ω=p/ρ$, whose range belongs to quintessence or even phantom matter.
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