发表机构
Indian Institute of Technology Guwahati; Indian Institute of Science（印度理工学院古瓦哈提分校; 印度科学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文研究再加热期间QCD轴子暗物质通过真空和动力学错位机制的产生，针对三种再加热情景确定满足观测遗迹密度和约束的参数空间，并评估轴子探测和引力波实验的探测潜力。
AI 中文摘要
我们研究了在慢滚暴涨结束后延长的再加热期间，通过真空错位和动力学错位机制产生QCD轴子暗物质（DM）的过程。考虑到暴涨前Peccei-Quinn对称性破缺，并假设再加热期间暴涨子势为单项式形式，我们将研究分为三种不同的微扰再加热情景：暴涨子衰变为（i）一对标准模型（SM）类玻色子，（ii）一对SM类费米子，或（iii）仅衰变为一对重右手中微子，后者在中间时期主导宇宙能量密度后最终衰变为SM末态。对于每种再加热情景，我们分别通过真空和动力学错位机制研究QCD轴子遗迹的细节。对于再加热、单项式暴涨子势和错位机制的不同组合，我们确定了与观测到的DM遗迹密度一致且满足其他宇宙学和实验室约束的参数空间。我们还检查了在轴子探测和引力波（GW）实验中探测当前允许参数空间的范围。
英文摘要
We study the production of QCD axion dark matter (DM) via vacuum and kinetic misalignment mechanisms during an extended reheating period after the end of slow-roll inflation. With pre-inflationary Peccei-Quinn breaking and considering a monomial inflaton potential during reheating, we classify our study into three different perturbative reheating scenarios in which the inflaton decays into (i) a pair of Standard Model (SM)-like bosons, (ii) a pair of SM-like fermions, or (iii) exclusively into a pair of heavy right-handed neutrinos, which eventually decays into the SM final states after dominating the energy density of the Universe for an intermediate epoch. For each of these reheating scenarios, we study the details of QCD axion relic separately via vacuum and kinetic misalignment mechanisms. For different combinations of reheating, monomial inflaton potential and misalignment mechanisms, we identify the parameter space consistent with the observed DM relic density while satisfying other cosmological and laboratory constraints. We also check the scope of probing the currently allowed parameter space at axion-detection and gravitational wave (GW) experiments.
Comments54 pages, 19 captioned figures
