AI 中文总结
本文研究非最小耦合标量-张量理论中的精质暴胀，通过双指数变形解决单一指数耦合无法提供晚期加速的矛盾，数值解得到解冻精质区域，未来暗能量测量可探测宇宙暴胀后再加热历史。
AI 中文摘要
我们在非最小耦合标量-张量理论中研究精质暴胀，对暴胀后的辐射丰度进行参数化，且不依赖于再加热机制。非绝热的暴胀-动能学转变会产生随机引力波背景，其对ΔN_eff的贡献对再加热温度设定了下限。由于该温度决定了动能学的持续时间和可用的标量场偏移量，因此它直接约束了现今的暗能量状态方程。单一指数耦合可实现所需的暴胀后势下降，但相同的常数斜率无法提供可行的晚期宇宙加速。双指数变形通过将控制总势下降的平均斜率与驱动宇宙加速的渐近斜率解耦，解决了这一矛盾。全数值解证实了这一图像，在我们的基准案例中产生了解冻精质区域，其w_φ,0≈(-0.90, -0.95)。我们的结果表明，未来的暗能量测量可以直接探测宇宙的暴胀后再加热历史。
英文摘要
We investigate quintessential inflation in a nonminimally coupled scalar-tensor theory, parameterizing the post-inflationary radiation abundance independently of the reheating mechanism. The nonadiabatic inflation-kination transition generates a stochastic gravitational-wave background whose contribution to $ΔN_{\textrm{eff}}$ imposes a lower limit on the reheating temperature. Because this temperature dictates the duration of kination and the available scalar-field excursion, it directly constrains the present-day dark-energy equation of state. While a single-exponential coupling achieves the required post-inflationary potential drop, the same constant slope does not provide viable late-time acceleration. A double-exponential deformation resolves this tension by decoupling the average slope governing the total potential drop from the asymptotic slope driving cosmic acceleration. Full numerical solutions confirm this picture, yielding a thawing quintessence regime with $w_{φ,0}\simeq (-0.90, -0.95)$ for our benchmarks. Our results demonstrate that future dark-energy measurements can directly probe the post-inflationary reheating history of the Universe.
Comments54 pages, 9 figures, 1 table, 1 appendix
