Quintessential Inflation in Palatini Gravity

Abstract

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 $T_{\mathrm{RH}}\sim \mathcal{O}(10^3-10^8)\mathrm{GeV}$, 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.

arXiv comment27 pages, 2 figures, 2 tables; v2: minor revision, references added, matches the published version

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• Extended interactions in the Palatini-$R^2$ inflation
• Inflation and reheating in quadratic metric-affine gravity with derivative couplings
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• Scalar-Induced Gravitational Waves in Palatini $f(R)$ Gravity
• Post-Newtonian Constraints on Scalar-Tensor Gravity