在具有负跑动的暖暴胀中阻止永恒暴胀
Defying eternal inflation in warm inflation with a negative running
AI总结：
本文将负谱指数跑动阻止永恒暴胀的结论推广至暖暴胀，发现其所需负跑动更小，且永恒暴胀的触发条件更严格。
摘要：
先前已有研究指出（Kinney:2014jya），来自（普通即冷）暴胀的曲率扰动谱指数若具有足够负的跑动，便能够阻止永恒暴胀发生。本文在暖暴胀背景下重新评估这些原始结果；在暖暴胀中，整个暴胀时期都存在由暴胀子产生的显著辐射组分。我们证明，在普通（冷）暴胀背景下发现的相同一般要求在暖暴胀中同样成立；事实上，只需更小量的负跑动便足以阻止永恒暴胀。这一点尤为切题，因为具有负跑动的模型在暖暴胀情景中更为普遍。最后，冷暴胀中永恒暴胀存在的条件——即曲率扰动振幅在超视界尺度上超过1——在暖暴胀情形下变得更具限制性。曲率扰动必须更大，也就是说，在势上要处于更远的位置，远离势中产生可观测信号（例如宇宙微波背景中的可观测信号）的部分。
英文摘要：
It was pointed out previously~\cite{Kinney:2014jya} that a sufficiently negative running of the spectral index of curvature perturbations from (ordinary i.e. cold) inflation is able to prevent eternal inflation from ever occurring. Here, we reevaluate those original results, but in the context of warm inflation, in which a substantial radiation component (produced by the inflaton) exists throughout the inflationary period. We demonstrate that the same general requirements found in the context of ordinary (cold) inflation also hold true in warm inflation; indeed an even tinier amount of negative running is sufficient to prevent eternal inflation. This is particularly pertinent, as models featuring negative running are more generic in warm inflation scenarios. Finally, the condition for the existence of eternal inflation in cold inflation -- that the curvature perturbation amplitude exceed unity on superhorizon scales -- becomes more restrictive in the case of warm inflation. The curvature perturbations must be even larger, i.e. even farther out on the potential, away from the part of the potential where observables, e.g. in the Cosmic Microwave Background, are produced.
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