Analytical investigation of pre-inflationary effects in the primordial power spectrum: from General Relativity to hybrid Loop Quantum Cosmology
Analytical investigation of pre-inflationary effects in the primordial power spectrum: from General Relativity to hybrid Loop Quantum Cosmology
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DOI：
10.1088/1475-7516/2021/09/030
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发表时间：
2021-04
影响因子：
6.4
通讯作者：
Beatriz Elizaga Navascués;G. A. Mena Marugán
中科院分区：
文献类型：
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作者：
Beatriz Elizaga Navascués;G. A. Mena Marugán
这项工作是对经典的快速滚转暴胀效应和混合环量子宇宙学（LQC）在原始功率谱上的印记之间的主要区别的分析研究。对现象感兴趣的有效LQC解决方案通常包含在慢滚膨胀之前的动能优势的经典时期，其功率谱的结果在这里我们试图将其与混合LQC中反弹附近发生的现象区分开来。为了进行比较，我们在相对论宇宙学和LQC宇宙学背景下使用相同的标准来选择原始扰动的真空状态。作为这个问题的第一个近似，我们的研究忽略了准德西特演化（而不是德西特）在慢滚动暴胀制度中的影响，以及在动力主导时代和慢滚动时期之间典型的短暂过渡。我们的研究结果表明，虽然这两种研究类型的效应可以导致光谱红外部分的剧烈功率抑制，但LQC发生这种情况的模式尺度要比经典相对论宇宙学大得多，相应的尺度分别与弹跳和暴胀开始时的时空曲率有关。
This work is an analytical study of the main differences between classical inflationary effects of a fast-roll regime and imprints of hybrid Loop Quantum Cosmology (LQC) on the primordial power spectrum. Effective LQC solutions of phenomenological interest typically contain a classical period of kinetic dominance prior to slow-roll inflation, with consequences on the power spectrum that here we try and tell apart from those of phenomena occuring in the vicinity of a bounce in hybrid LQC. For this comparison, we use the same criterion for the choice of a vacuum state of the primordial perturbations, both in the context of relativistic cosmology and on the LQC cosmological background. As a first approximation to the problem, our study ignores the influence of a quasi-de Sitter evolution (rather than de Sitter) in the slow-roll inflationary regime, and of a typically short transition between the kinetically dominated era and the slow-roll period. Our results show that, while the two studied types of effects can lead to a drastic power suppression in the infrared sector of the spectrum, the mode scale at which this happens is much larger for LQC than for classical relativistic cosmology, the corresponding scales being related to the spacetime curvature at the bounce and at the onset of inflation, respectively.