Two-field K\"ahler moduli inflation on large volume moduli stabilization

TL;DR

This paper introduces a two-field inflation model derived from large volume moduli stabilization in type IIB string theory, featuring a non-canonical kinetic term and producing observable cosmological signatures.

Contribution

It presents a novel two-field inflation scenario with a non-canonical kinetic Lagrangian based on large volume moduli stabilization in string theory.

Findings

Achieves a nearly flat power spectrum with n_s≈0.96.

Predicts an inflationary energy scale of 3×10^{14} GeV.

Finds significant correlation between curvature and isocurvature perturbations.

Abstract

In this paper we present a two-field inflation model, which distinguishes itself with a non-canonical kinetic lagrangian and comes from the large volume approach to the moduli stabilization in flux compactification of type IIB superstring on a Calabi-Yau orientifold of $h^{(1,2)} > h^{(1,1)}\geq 4$. The K\"ahler moduli are classified as volume modulus, heavy moduli and two light moduli. The axion-dilaton, complex structure moduli and all heavy K\"ahler moduli including the volume modulus are frozen by nonperturbatively corrected flux superpotential and the $\alpha^\prime$-corrected K\"ahler potential in the large volume limit. The minimum of the scalar potential at which the heavy moduli are stabilized provides the dominant potential energy for the survived light K\"ahler moduli. We consider a simplified case where the axionic components in the light K\"ahler moduli are further stabilized at the potential minimum and only the geometrical components are taken as the scalar fields to drive an assisted-like inflation. For a certain range of moduli stabilization parameters and inflation initial conditions, we obtain a nearly flat power spectrum of the curvature perturbation, with $n_s\approx 0.96$ at Hubble-exit, and an inflationary energy scale of $3 \times 10^{14}$ GeV. In our model, significant correlation exists between the curvature and isocurvature perturbations on super-Hubble scales so that at the end of inflation a great deal of the curvature power spectrum originates from this correlation.