# Inflation in Loop Quantum Cosmology

## TL;DR

This paper develops an analytic framework for understanding how slow-roll inflation can emerge in Loop Quantum Cosmology, considering various initial conditions and potentials, and compares results with numerical simulations.

## Contribution

It provides the first comprehensive analytic analysis of inflation conditions in LQC, including different initial regimes and potential types, with validation against numerical results.

## Key findings

- Superinflation phase occurs in kinetic dominated regimes.
- Slow-roll inflation naturally follows damping phases in certain scenarios.
- Analytic results agree well with numerical simulations, enabling further perturbation analysis.

## Abstract

We develop a consistent analytic approach to determine the conditions under which slow roll inflation can arise when the inflaton is the same scalar field that is responsible for the bounce in Loop Quantum Cosmology (LQC). We find that the requirement that the energy density of the field is fixed at the bounce having to match a critical density has important consequences for its future evolution. For a generic potential with a minimum, we find different scenarios depending on the initial velocity of the field and whether it begins life in a kinetic or potential energy dominated regime. For chaotic potentials that start in a kinetic dominated regime, we find an initial phase of superinflation independent of the shape of the potential followed by a damping phase which slows the inflaton down, forcing it to turnaround and naturally enter a phase of slow-roll inflation. If we begin in a potential energy dominated regime, then the field undergoes a period where the corrections present in LQC damp its evolution once again forcing it to turnaround and enter a phase of slow roll inflation. On the other hand we show for the Starobinsky potential that inflation never occurs when we begin in a potential dominated regime. In fact traditional Starobinsky inflation has to start in a kinetic energy dominated regime, with corresponding tighter constraints on the initial value of the field for successful inflation than in the conventional case. Comparing our analytic results to published numerical ones, we find remarkable agreement especially when we consider the different epochs that are involved. In particular the values of key observables obtained from the two approaches are in excellent agreement, opening up the possibility of obtaining analytic results for the evolution of the density perturbations in these models.