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  • 1706.09735

    Rights statement: This is the author’s version of a work that was accepted for publication in Astroparticle Physics. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Astroparticle Physics, 103, 2018 DOI: 10.1016/j.astropartphys.2018.06.002

    Accepted author manuscript, 563 KB, PDF document

    Available under license: CC BY-NC-ND: Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License

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Loop inflection-point inflation

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Published
<mark>Journal publication date</mark>12/2018
<mark>Journal</mark>Astroparticle Physics
Volume103
Number of pages5
Pages (from-to)16-20
Publication StatusPublished
Early online date14/06/18
<mark>Original language</mark>English

Abstract

A novel inflection-point inflation model is analysed. The model considers a massless scalar field, whose self-coupling’s running is stabilised by a non-renormalisable operator. The running is controlled by a fermion loop. We find that successful inflation is possible for a natural value of the Yukawa coupling y≃4×10^{−4}. The necessary fine-tuning is only ∼10^{−6}, which improves on the typical tuning of inflection-point inflation models, such as MSSM inflation. The model predicts a spectral index within the 1-σ bound of the latest CMB observations, with a very small negative running, and negligible tensors (r∼10^{−(9−10)}). These results are largely independent of the order of the stabilising non-renormalisable operator.

Bibliographic note

This is the author’s version of a work that was accepted for publication in Astroparticle Physics. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Astroparticle Physics, 103, 2018 DOI: 10.1016/j.astropartphys.2018.06.002