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arXiv 2110.01482gr-qchep-phhep-th
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原初黑洞在$α$ -吸引子暴胀中产生的非高斯性和次级引力波

Non-Gaussianity and Secondary Gravitational Waves from Primordial Black Holes Production in $α$-attractor Inflation

Kazem Rezazadeh, Zeinab Teimoori, Saeid Karimi, Kayoomars Karami

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38 pages, 9 figures
发表信息：
Eur. Phys. J. C 82, 758 (2022)
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摘要：

研究了暴胀产生原初黑洞过程中的非高斯性和次级引力波。在我们的工作中，我们专注于$α$ -吸引子暴胀模型，其中暴胀子势中的微小凸起在某些尺度上增强了曲率扰动的幅度，从而导致不同质量尺度的PBH产生。我们实现了计算程序BINGO，计算不同三角形配置下的非高斯参数。我们的研究表明，在这种设置中，非高斯性得到放大显着的等边形状周围的标量扰动的功率谱经历了急剧下降的尺度。这些非高斯性的印记可以在对应于BBN和$μ$ -失真事件的尺度中探测，或者在更小的尺度中探测，并且在未来的观测中检测到这样的签名可以证实我们的模型用于生成PBH的想法或者排除它。此外，我们研究了在这个框架下的次级GWs，并表明，在我们的模型中，目前的分数能量密度的峰值是在不同的频率，这取决于模型参数的$Ω_{\rm GW0} \sim 10^{-8}$。这些结果在某些频率下处于某些GWs探测器的敏感区域内，因此我们模型的观测兼容性可以通过这些探测器即将获得的数据来评估。我们进一步估计了不同频率区间上的诱导GWs谱的倾斜度，并证明了在这些频率区间上诱导GWs谱服从幂律关系$Ω_{\rm GW0}\sim f^{n}$。

英文摘要：

We study the non-Gaussianity and secondary Gravitational Waves (GWs) in the process of the Primordial Black Holes (PBHs) production from inflation. In our work, we focus on the $α$-attractor inflation model in which a tiny bump in the inflaton potential enhances the amplitude of the curvature perturbations at some scales and consequently leads to the PBHs production with different mass scales. We implement the computational code BINGO which calculates the non-Gaussianity parameter in different triangle configurations. Our examination implies that in this setup, the non-Gaussianity gets amplified significantly in the equilateral shape around the scales in which the power spectrum of the scalar perturbations undergoes a sharp declination. The imprints of these non-Gaussianities can be probed in the scales corresponding to the BBN and $μ$-distortion events, or in smaller scales, and detection of such signatures in the future observations may confirm the idea of our model for the generation of PBHs or rule it out. Moreover, we investigate the secondary GWs in this framework and show that in our model, the peak of the present fractional energy density is obtained as $Ω_{\rm GW0} \sim 10^{-8}$ at different frequencies which depends on the model parameters. These results lie well within the sensitivity region of some GWs detectors at some frequencies, and therefore the observational compatibility of our model can be evaluated by the forthcoming data from these detectors. We further provide some estimations for the tilts of the induced GWs spectrum in the different intervals of frequency, and demonstrate that the spectrum obeys the power-law relation $Ω_{\rm GW0}\sim f^{n}$ in those frequency bands.

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