AI 中文总结
该研究构建了非最小引力耦合复暴胀子驱动暴胀的微扰框架，其在暴胀末期激活非厄米部分触发几何 reheating，使高频引力波谱出现独特抑制，有望被未来探测器检验。
AI 中文摘要
本研究针对由具有非最小引力耦合和非厄米势的复暴胀子驱动的暴胀，构建了一个微扰框架。在可观测的宇宙微波背景辐射时代，该动力学简化为一个有效保守的双场模型，保留了α吸引子类的预测，并满足普朗克2018以及BICEP/Keck对$n_s$、$r$和$f_{\rm NL}$的约束。在暴胀末期，轨迹弯曲激活非厄米部分，触发几何 reheating。由此产生的非幺正演化通过由复质量本征值确定的可计算阻尼因子修改曲率谱和随机引力波背景。虽然宇宙微波背景尺度的可观测量基本保持不变，但在高频引力波谱（$f > 10^2$ Hz）中出现了独特的抑制，这可能通过未来的探测器如爱因斯坦望远镜和大爆炸观测者进行检验。
英文摘要
In this work, we develop a perturbative framework for inflation driven by a complex inflaton with non-minimal gravitational coupling and a non-Hermitian potential. During the observable cosmic microwave background radiation era, the dynamics reduce to an effectively conservative two-field model, preserving the predictions of the $α$-attractor class and satisfying Planck 2018 and BICEP/Keck constraints on $n_s$, $r$, and $f_{\mathrm{NL}}$. Near the end of inflation, trajectory bending activates the non-Hermitian sector, triggering geometric reheating. The resulting non-unitary evolution modifies the curvature spectrum and stochastic gravitational-wave background through a calculable damping factor determined by the complex mass eigenvalues. While cosmic microwave background-scale observables remain essentially unchanged, a distinctive suppression emerges in the high-frequency gravitational-wave spectrum ($f > 10^2$ Hz), potentially testable by future detectors such as the Einstein Telescope and the Big Bang Observer.
