2004/01/15 by M. G. Barnett, Rainer Dick, R. Dick +2 · 1 citation
Physics and Astronomy · #Astrophysics #Cosmology #Cosmology and Gravitation Theories #Coupling (piping) #Coupling constant #Dark Matter and Cosmic Phenomena #Dark energy #Dark matter #Electron #Field (mathematics) #Fine-structure constant #Mathematical physics #Particle physics theoretical and experimental studies #Physics #Planck #Quantum mechanics #Scalar field #Spectral line #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.07625.x
published as Mon.Not.Roy.Astron.Soc. 349 (2004) 1500 · 6 pages, accepted for publication in the MNRAS
arxiv created 2004/01/15 · openalex publication_date 2004/04/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We consider the problem of the evolution of the fine-structure coefficient α under the assumption that the scalar field coupling to the Maxwell term satisfies the condition mt≫ 1 for coherent dark matter oscillations. In this case we find that the coupling scale f in the leading-order coupling −(φ/4f) FμνFμν affects the cosmological evolution of α according to ln(α/α0) ∝ξ(mPl/f) × ln [tanh(t/2τ)/tanh(t0/2τ)]. A fit to the QSO observations by Murphy et al. yields f=ξ× 2.12+0.58−0.37× 105mPl. Here mPl= (8πGN)−1/2 is the reduced Planck mass, and ξ2=ϱφ/ϱm parametrizes the contribution of φ to the matter density in the Universe.