标题： 从带有粒子产生的爱因斯坦-卡特-斯恰马-基布尔引力中重建暴涨子势能的非参数方法 显示英文标题

标题： Non-parametric reconstruction of an inflaton potential from Einstein-Cartan-Sciama-Kibble gravity with particle production

摘要： 在爱因斯坦-卡特兰-斯恰马-基布尔引力理论中，自旋与挠率之间的耦合在极高密度下产生引力排斥力，这可以防止黑洞中出现奇点，并可能在那里创造一个新宇宙。 我们证明，在这种宇宙中接近最后一次反弹（代表大爆炸）时的量子粒子产生，给出了动力学机制，解决了宇宙学中的视界、平坦性以及同质性问题。 对于粒子产生系数的特定范围，我们得到一个几乎恒定的哈勃参数，它使宇宙以超过60个$e$倍的增长率进行指数膨胀，持续时间约为$\sim 10^{-42}$秒。因此，这一情景可以解释宇宙膨胀而不需引入基本标量场和再加热过程。 从尺度因子的时间依赖关系中，我们遵循埃利斯和马德森的建议，用非参数化的方法重构出一个标量场势能，该势能给出早期宇宙相同的动力学。 此势能提供了宇宙膨胀的慢滚参数，从中我们计算了张量-标量比、密度扰动的标量谱指数及其运行，作为生产系数的函数。 我们发现这些量在大反弹处并不显著依赖于尺度因子。 我们对这些量的预测与普朗克2015年的观测结果一致。 显示英文摘要

摘要： The coupling between spin and torsion in the Einstein-Cartan-Sciama-Kibble theory of gravity generates gravitational repulsion at very high densities, which prevents a singularity in a black hole and may create there a new universe. We show that quantum particle production in such a universe near the last bounce, which represents the Big Bang gives the dynamics that solves the horizon, flatness, and homogeneity problems in cosmology. For a particular range of the particle production coefficient, we obtain a nearly constant Hubble parameter that gives an exponential expansion of the universe with more than 60 $e$-folds, which lasts about $\sim 10^{-42}$ s. This scenario can thus explain cosmic inflation without requiring a fundamental scalar field and reheating. From the obtained time dependence of the scale factor, we follow the prescription of Ellis and Madsen to reconstruct in a non-parametric way a scalar field potential which gives the same dynamics of the early universe. This potential gives the slow-roll parameters of cosmic inflation, from which we calculate the tensor-to-scalar ratio, the scalar spectral index of density perturbations, and its running as functions of the production coefficient. We find that these quantities do not significantly depend on the scale factor at the Big Bounce. Our predictions for these quantities are consistent with the Planck 2015 observations.