关于大尺度结构有效场论的重整化
On the Renormalization of the Effective Field Theory of Large Scale Structures
摘要：
大尺度物质非均匀性的标准微扰理论（SPT）至少有三个原因不能令人满意：没有明确的膨胀参数，因为密度对比在所有尺度上都不小;它不能完全解释大尺度下由短尺度非线性引起的与理想无压流体的偏差;对于一般的初始条件，环路修正是UV发散的，使得预测依赖于截止点，因此是非物理的。大尺度结构的有效场论成功地解决了这三个问题。在这里，我们专注于第三个，并明确表明，在SPT中被忽略的短尺度积分所引起的项，具有完全正确的尺度依赖性，以消除一个循环中的所有UV发散，这应该在所有循环中保持。一个特别明显的例子是具有无标度初始条件P_in=A k^n的爱因斯坦deSitter宇宙。在对理论进行重新规范化之后，我们使用自相似性来导出任何n的最终功率谱的非常简单的结果，不包括双回路校正和更高的校正。我们展示了不同校正的相对重要性如何依赖于n。当n=-1.5时，与我们的宇宙相关，压力和耗散修正比双环修正更重要。
英文摘要：
Standard perturbation theory (SPT) for large-scale matter inhomogeneities is unsatisfactory for at least three reasons: there is no clear expansion parameter since the density contrast is not small on all scales; it does not fully account for deviations at large scales from a perfect pressureless fluid induced by short-scale non-linearities; for generic initial conditions, loop corrections are UV-divergent, making predictions cutoff dependent and hence unphysical. The Effective Field Theory of Large Scale Structures successfully addresses all three issues. Here we focus on the third one and show explicitly that the terms induced by integrating out short scales, neglected in SPT, have exactly the right scale dependence to cancel all UV-divergences at one loop, and this should hold at all loops. A particularly clear example is an Einstein deSitter universe with no-scale initial conditions P_in=A k^n. After renormalizing the theory, we use self-similarity to derive a very simple result for the final power spectrum for any n, excluding two-loop corrections and higher. We show how the relative importance of different corrections depend on n. For n=-1.5, relevant for our universe, pressure and dissipative corrections are more important than the two-loop corrections.
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。
