We study perturbative reheating at the end of fibre inflation where the inflaton is a closed string modulus with a Starobinsky-like potential. We first derive the spectral index n s and the tensor-to-scalar ratio r as a function of the number of efoldings and the parameter R which controls slow-roll breaking corrections. We then compute the inflaton couplings and decay rates into ultra-light bulk axions and visible sector fields on D7-branes wrapping the inflaton divisor. This leads to a reheating temperature of order 10 10 GeV which requires 52 efoldings. Ultra-light axions contribute to dark radiation even if Δ N eff is almost negligible in the generic case where the visible sector D7-stack supports a non-zero gauge flux. If the parameter R is chosen to be small enough, n s 0.965 is then in perfect agreement with current observations while r turns out to be of order r 0.007. If instead the flux on the inflaton divisor is turned off, Δ N eff 0.6 which, when used as a prior for Planck data, requires n s 0.99. After R is fixed to obtain such a value of n s , primordial gravity waves are larger since r 0.01.

Reheating and dark radiation after fibre inflation

Cicoli M.
Supervision
;
2019

Abstract

We study perturbative reheating at the end of fibre inflation where the inflaton is a closed string modulus with a Starobinsky-like potential. We first derive the spectral index n s and the tensor-to-scalar ratio r as a function of the number of efoldings and the parameter R which controls slow-roll breaking corrections. We then compute the inflaton couplings and decay rates into ultra-light bulk axions and visible sector fields on D7-branes wrapping the inflaton divisor. This leads to a reheating temperature of order 10 10 GeV which requires 52 efoldings. Ultra-light axions contribute to dark radiation even if Δ N eff is almost negligible in the generic case where the visible sector D7-stack supports a non-zero gauge flux. If the parameter R is chosen to be small enough, n s 0.965 is then in perfect agreement with current observations while r turns out to be of order r 0.007. If instead the flux on the inflaton divisor is turned off, Δ N eff 0.6 which, when used as a prior for Planck data, requires n s 0.99. After R is fixed to obtain such a value of n s , primordial gravity waves are larger since r 0.01.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/695702
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