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arXiv 1407.7325astro-ph.COgr-qc
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一般暗能量模型中的精确三阶密度微扰和单圈功率谱

Exact Third-Order Density Perturbation and One-Loop Power Spectrum in General Dark Energy Models

Seokcheon Lee, Changbom Park, Sang Gyu Biern

备注：
13pages, 5figures, accepted by PLB
发表信息：
Physics Letters B, Volume 736, p. 403-410 (2014)
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摘要：

在标准微扰理论（SPT）下，首次在不使用Einstein-de Sitter（EdS）宇宙假设的情况下，得到了一般暗能量模型的完全一致的三阶密度涨落和核.我们还表明，即使时间和空间分量的SPT解决方案不能分开，人们可以找到任何顺序的一般暗能量模型的精确解。利用这些精确解，我们得到了一圈物质功率谱的误差修正小于EDS假设下$k = 0.1 {\rm h\, Mpc}^{-1}$模在$z = 0$（1，1.5）处的误差修正.因此，EdS假设在这个规模下工作得很好。然而，如果考虑对$P_{13}$的校正，则对于$z = 0$（1，1.5）处的相同模式，误差约为6（9，11）\%。在重整化微扰理论（RPT）中，人们把$P_{13}$吸收到线性功率谱中，因此应该使用精确解而不是近似解。对于$k = 0.4 {\rm h\, Mpc}^{-1}$，在$z =0$（1，1.5）处，RPT的迭代传播子$N$的误差约为14（8，6）%.对于$k = 1 {\rm h\, Mpc}^{-1}$，总物质功率谱在$z = 0$（1，1.5）处的误差修正约为3.6（4.6，4.5）%.接下来的观测需要达到亚百分比的精度，以提供对暗能量的强约束，这种一致的解决方案是模型比较的先决条件。

英文摘要：

Under the standard perturbation theory (SPT), we obtain the fully consistent third-order density fluctuation and kernels for the general dark energy models without using the Einstein-de Sitter (EdS) universe assumption for the first time. We also show that even though the temporal and spatial components of the SPT solutions can not be separable, one can find the exact solutions to any order in general dark energy models. With these exact solutions, we obtain the less than \% error correction of one-loop matter power spectrum compared to that obtained from the EdS assumption for $k = 0.1 {\rm h\, Mpc}^{-1}$ mode at $z = 0$ (1, 1.5). Thus, the EdS assumption works very well at this scale. However, if one considers the correction for $P_{13}$, the error is about 6 (9, 11) \% for the same mode at $z = 0$ (1, 1.5). One absorbs $P_{13}$ into the linear power spectrum in the renormalized perturbation theory (RPT) and thus one should use the exact solution instead of the approximation one. The error on the resummed propagator $N$ of RPT is about 14 (8, 6) \% at $z =0$ (1, 1.5) for $k = 0.4 {\rm h\, Mpc}^{-1}$. For $k = 1 {\rm h\, Mpc}^{-1}$, the error correction of the total matter power spectrum is about 3.6 (4.6, 4.5) \% at $z = 0$ (1, 1.5). Upcoming observation is required to archive the sub-percent accuracy to provide the strong constraint on the dark energy and this consistent solution is prerequisite for the model comparison.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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