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• W2058232471 abstract "We consider the classical evolution of the inflaton field $phi(t)$ and the Hubble parameter $H(t)$ in homogeneous and isotropic single-field inflation models. Under an extremely broad assumption, we show that the universe generically emerges from an initial singularity in a non-inflating state where the kinetic energy of the inflaton dominates its potential energy, $dot{phi}^2 gg V(phi)$. In this kinetically-dominated regime, the dynamical equations admit simple analytic solutions for $phi(t)$ and $H(t)$, which are independent of the form of $V(phi)$. In such models, these analytic solutions thus provide a simple way of setting the initial conditions from which to start the (usually numerical) integration of the coupled equations of motion for $phi(t)$ and $H(t)$. We illustrate this procedure by applying it to spatially-flat models with polynomial and exponential potentials, and determine the background evolution in each case; generically $H(t)$ and $|phi(t)|$ as well as their time derivatives decrease during kinetic dominance until $dot{phi}^2sim V(phi)$, marking the onset of a brief period of fast-roll inflation prior to a slow roll phase. We also calculate the approximate spectrum of scalar perturbations produced in each model and show that it exhibits a generic damping of power on large scales. This may be relevant to the apparent low-$ell$ falloff in the CMB power spectrum." @default.
• W2058232471 created "2016-06-24" @default.
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• W2058232471 date "2014-03-06" @default.
• W2058232471 modified "2023-09-24" @default.
• W2058232471 title "Kinetic initial conditions for inflation" @default.
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• W2058232471 doi "https://doi.org/10.1103/physrevd.89.063505" @default.
• W2058232471 hasPublicationYear "2014" @default.
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