Reheating in tachyonic inflationary models: Effects on the large scale curvature perturbations

TL;DR

This study examines how reheating after tachyonic inflation influences large-scale curvature perturbations, finding that reheating does not alter their amplitude, supported by numerical analysis of perturbation evolution across different potentials and decay scenarios.

Contribution

It provides a detailed numerical investigation of perturbation evolution during reheating in tachyonic inflation, demonstrating the invariance of curvature perturbations' amplitude.

Findings

Reheating does not affect the amplitude of curvature perturbations.

Non-adiabatic pressure perturbations decay rapidly after the transition.

Results are consistent across different tachyon potentials and decay types.

Abstract

We investigate the problem of perturbative reheating and its effects on the evolution of the curvature perturbations in tachyonic inflationary models. We derive the equations governing the evolution of the scalar perturbations for a system consisting of a tachyon and a perfect fluid. Assuming the perfect fluid to be radiation, we solve the coupled equations for the system numerically and study the evolution of the perturbations from the sub-Hubble to the super-Hubble scales. In particular, we analyze the effects of the transition from tachyon driven inflation to the radiation dominated epoch on the evolution of the large scale curvature and non-adiabatic pressure perturbations. We consider two different tachyonic potentials and study the effects of two possible types of decay of the tachyon into radiation. We plot the spectrum of curvature perturbations at the end of inflation as well as at the early stages of the radiation dominated epoch. We find that reheating does not affect the amplitude of the curvature perturbations in any of these cases. These results corroborate similar conclusions that have been arrived at earlier based on the study of the evolution of the perturbations in the super-Hubble limit. We illustrate that, before the transition to the radiation dominated epoch, the relative non-adiabatic pressure perturbation between the tachyon and radiation decays in a fashion very similar to that of the intrinsic entropy perturbation associated with the tachyon. Moreover, we show that, after the transition, the relative non-adiabatic pressure perturbation dies down extremely rapidly during the early stages of the radiation dominated epoch. These behavior ensure that the amplitude of the curvature perturbations remain unaffected during reheating. We also discuss the corresponding results for the popular chaotic inflation model in the case of the canonical scalar field. [abridged]