QCD axions and CMB anisotropy

2020/07/31 by Satoshi Iso, Kiyoharu Kawana, Kengo Shimada · 2 citations
Physics and Astronomy · #Anisotropy #Astrophysics #Axion #Cosmic microwave background #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Inflation (cosmology) #Inflaton #Particle physics #Particle physics theoretical and experimental studies #Physics #Quantum chromodynamics #Quantum electrodynamics #Quantum mechanics #Strong CP problem #Theoretical physics #Universe #astro-ph.CO #hep-ph #hep-th

paper · pdf · doi:10.1103/physrevd.102.103513

published in Physical review. D/Physical review. D. 102(10), 103513 (American Physical Society) · 39 pages, 5 figures; version to appear in PRD (v2)

arxiv created 2020/10/20 · openalex publication_date 2020/11/12 · arxiv updated 2020/11/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

In this paper, we consider a possibility that the temperature anisotropy of cosmic microwave background (CMB) is dominantly generated by the primordial fluctuations of QCD-axion like particles under a circumstance that inflaton's perturbation is too small to explain the CMB anisotropy. Since the axion potential is generated by acquiring its energy from radiation, the primordial fluctuations of the axion field generated in the inflation era are correlated with the CMB anisotropies. Consequently, the observations stringently constrain a model of the axion and the early Universe scenario. The following conditions must be satisfied: (i) sufficient amplitudes of the CMB anisotropy (ii) consistency with the axion isocurvature constraint and (iii) the non-Gaussianity constraint. To satisfy these conditions, a large energy fraction \mathrm\ensuremathΩ_A of the axion is necessary at the QCD scale when the axion-potential is generated, but simultaneously, it must become tiny at the present era due to the isocurvature constraint. Thus, an additional scenario of the early Universe, such as low scale thermal inflation, is inevitable to dilute the axions after the QCD scale. We investigate such a model and obtain its allowed parameter region.

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