论文标题
Palatini重力的典型通货膨胀
Quintessential Inflation in Palatini Gravity
论文作者
论文摘要
我们研究了在Palatini重力背景下进行典型通货膨胀的模型。作为一个代表性的例子，我们考虑了典型通货膨胀的Peebles-Vilenkin模型，其与重力相对于重力小小，这与最新的Planck测量值一致。在通货膨胀结束时，充气场通过了速旋区，并通过次要的预热过程导致爆炸性颗粒的产生。预热后，宇宙被充气的动能统治，并进入了一段时期。最终，宇宙的总能量密度由辐射占主导地位，导致重新加热。我们发现该模型可以预测重新加热的温度值$ t _ {\ rm {rm {rm {rm sim \ sim \ Mathcal {o}（10^3-10^8）\，\ rm {gev} $，它显着高于大爆炸核合成的温度。重新加热后，充气场降低了典型的潜力，直到冻结为止。由于典型性一直冷冻到今天，因此该磁场值的残余势能密度解释了观察到的黑能密度。
We study a model of quintessential inflation in the context of Palatini gravity. As a representative example, we consider the Peebles-Vilenkin model of quintessential inflation with a small non-minimal coupling to gravity, which is consistent with the most recent Planck measurements. At the end of inflation, the inflaton field passes through a tachyonic region and it leads to explosive particle production through the tachyonic preheating process. After preheating, the Universe becomes dominated by the kinetic energy of the inflaton and enters a period of kination. Eventually, the total energy density of the Universe becomes dominated by radiation, resulting in reheating. We find that the model predicts the reheating temperature values $T_{\rm{RH}} \sim \mathcal{O}(10^3 - 10^8) \, \rm{GeV}$, which is significantly above the temperature of Big Bang Nucleosynthesis. Following reheating, the inflaton field rolls down the quintessence potential until it freezes. Since the quintessence remains frozen until the present day, the residual potential energy density at this field value explains the observed dark energy density.
