arXiv 2205.005752022-05gr-qchep-th

一个阶跃混沌势的暴胀

Inflation from a chaotic potential with a step

Clara Rojas, Rafael Hernández-Jiménez

备注：: 21 pages, 16 figures
发表信息：: Phys. Dark Univ. 40 (2023) 101188
DOI：: 10.1016/j.dark.2023.101188

摘要：

本文研究了带阶跃的混沌势对暴胀宇宙相关观测参数的影响。我们数值演化的扰动方程在冷膨胀和暖膨胀。一方面，在冷暴胀场景中，我们根据e折叠$N_{e}$的数量和比率$k/k_{0}$来分析标量功率谱$P_{\mathcal{R}}$，其中$k_{0}$是我们的枢轴尺度。我们展示了$P_{\mathcal{R}}$如何围绕$0.2< k/k_{0} < 20$振荡。此外，我们提出了两个相关参数的演变：标量谱指数$n_\mathrm{s}$和张量标量比$r$。事实上，$(n_\mathrm{s},r)$的不止一个区域位于可观测窗口内（普朗克2018）。另一方面，在暖暴胀的情形下，我们也用$N_{e}$和$k/k_{0}$检验了$P_{\mathcal{R}}$的演化。WI中的扰动被放大;事实上，$P_{\mathcal{R}}$可能远大于CMB值$P_{\mathcal{R}}> 2.22\times 10^{-9}$。这一次，光谱指数$n_\mathrm{s}$在较小的尺度上明显是蓝倾斜的，并且张量与标量之比$r$变得太低。然而，$n_\mathrm{s}$可以从蓝色倾斜变为红色倾斜，因为$P_{\mathcal{R}}$开始围绕$k/k_{0}\sim 40$振荡。实际上，阶跃势的结果与普朗克轮廓不符。最后，本研究的一个关键方面是对比两种范式之间的通货膨胀潜力的特征，事实上，它们表现出相似性和差异性。由于一个特殊的背景和熵涨落的综合效应（仅在暖暴胀中），在这两种情况下，某些涨落尺度在超视界尺度上不再“冻结”。

英文摘要：

In this work, we study the effects on the relevant observational parameters of an inflationary universe from a chaotic potential with a step. We numerically evolve the perturbation equations within both cold inflation and warm inflation. On the one hand, in a cold inflation scenario we analyse the scalar power spectrum $P_{\mathcal{R}}$ in terms of the number of e-folds $N_{e}$, and in terms of the ratio $k/k_{0}$, where $k_{0}$ is our pivot scale. We show how $P_{\mathcal{R}}$ oscillates around $0.2< k/k_{0} < 20$. Additionally, we present the evolution of two relevant parameters: the scalar spectral index $n_\mathrm{s}$ and the tensor-to-scalar ratio $r$. In fact, more than one region of $(n_\mathrm{s},r)$ lies within the observable window (Planck 2018). On the other hand, in the warm inflationary case, we also examine the evolution of $P_{\mathcal{R}}$ in terms of $N_{e}$ and $k/k_{0}$. Perturbations are amplified in WI; in fact, $P_{\mathcal{R}}$ can be much larger than the CMB value $P_{\mathcal{R}}> 2.22\times 10^{-9}$. This time, the spectral index $n_\mathrm{s}$ is clearly blue-tilted, at smaller scales, and the tensor-to-scalar ratio $r$ becomes too low. However, $n_\mathrm{s}$ can change from blue-tilted towards red-tilted, since $P_{\mathcal{R}}$ starts oscillating around $k/k_{0}\sim 40$. Indeed, the result from the step potential skims the Planck contours. Finally, one key aspect of this research was to contrast the features of an inflationary potential between both paradigms, and, in fact, they show similarities and differences. Due to a featured background and a combined effect of entropy fluctuations (only in warm inflation), in both scenarios certain fluctuation scales are not longer ``freeze in'' on super-horizon scales.

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。

摘要：

英文摘要：

相关论文