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Three-field string inflation with perturbative corrections: Dynamics and implications

Vasileios Basiouris1,* and Dibya Chakraborty2,†

  • *Contact author: v.basiouris@uoi.gr, v.basiouris@gmail.com
  • †Contact author: dibyac@physics.iitm.ac.in
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Phys. Rev. D 111, 126008 – Published 13 June, 2025

DOI: https://doi.org/10.1103/7bkz-kty3

Abstract

In this work, we construct an explicit string motivated example of three-field inflation related to, yet distinct from the recently discovered perturbative large volume scenario (pLVS). In this setup, large volume is ensured by the interplay between the effects of α′3, logarithmic loop, and higher derivative F4 corrections. After addressing full moduli stabilization, we move on to a detailed analysis of a three-field model of inflation while choosing a suitable canonical basis for the fields. Our model differs from previous setups in three key aspects: first, the interaction between subleading corrections that drive full moduli stabilization is different compared to pLVS for instance; second, the volume of the underlying Calabi-Yau is of “weak-Swiss-cheese” type; and third, in our three-field inflationary scenario, the second Hubble slow-roll parameter consistently dominates over the first by several orders of magnitude—primarily due to the steepness of the potential. When this hierarchy is aided by a brief deviation from slow roll, an enhancement in the primordial power spectrum can be naturally achieved. We have obtained two stages of inflation: the first stage mostly occurs when one of the inflatons roll along the steepest direction—completing 55 e-folds of inflation. Once the rolling inflaton falls off a ridge of the multifield potential, the other two fields become active, giving us a true multifield behavior in the second stage—adding few more e-folds of inflation. Inflation ends when all three of them roll toward the global minimum and settle there. We confirm this behavior by introducing the nonplanar torsion in the inflationary trajectory—this quantity becomes nontrivial in the second stage of inflation. Finally, we calculate the cosmological observables, which align with the Planck data, and discuss potential directions for future research.

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Phys. Rev. D 111, 126008– Published 13 June, 2025
  • Received 25 February 2025
  • Accepted 21 May 2025
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