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Dynamics of Peccei-Quinn Breaking Field after Inflation and Axion Isocurvature Perturbations

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arxiv 1507.00119 v1 pith:RSXRIQ7D submitted 2015-07-01 hep-ph astro-ph.CO

Keisuke Harigaya , Masahiro Ibe , Masahiro Kawasaki , Tsutomu T. Yanagida This is my paper
classification hep-phastro-ph.CO
keywords peccei-quinnbreakinginflationfieldisocurvatureperturbationsdiscussdomain
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The Peccei-Quinn mechanism suffers from the problem of the isocurvature perturbations. The isocurvature perturbations are suppressed if the Peccei-Quinn breaking scale is large during inflation. The oscillation of the Peccei-Quinn breaking field after inflation, however, leads to the formation of domain walls due to the parametric resonance effect. In this paper, we discuss the evolution of the Peccei-Quinn breaking field after inflation in detail, and propose a model where the parametric resonance is ineffective and hence domain walls are not formed. We also discuss consistency of our model with supersymmetric theory.

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Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Axion isocurvature and the model-building problem of low-scale inflation

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    Radion dynamics in warped 5D models enhance the axion decay constant during inflation, satisfying CMB isocurvature bounds at higher Hubble scales while restoring the QCD window afterward.

  3. Transient Bias for CP Domain Wall Decay and Dark Matter

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  4. Axions on a Hyperbolic Ride: Geometric Suppression of CMB Isocurvature and a Blue-Tilted Spectrum

    hep-ph 2026-01 conditional novelty 6.0 of 10

    A hyperbolic PQ field-space metric exponentially suppresses CMB axion isocurvature and induces a blue-tilted spectrum, allowing H_inf≈10^13 GeV with fa up to 10^16 GeV.

  5. Bias with a Timer: Axion Domain Wall Decay and Dark Matter

    hep-ph 2025-07 conditional novelty 6.0 of 10

    A light spectator field first creates and later disables an extra axion potential, letting axion domain walls decay and matching dark matter at larger decay constants.

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