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Cosmological Magnetic Fields from Ultralight Dark Matter
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abstract
We propose a mechanism for the generation of magnetic fields on cosmological scales that is operative after recombination. An essential ingredient is an instability (of parametric resonance type) of the electromagnetic field driven by an oscillating pseudo-scalar dark matter field, $\phi$, that is coupled to the electromagnetic field tensor via a $\phi F \wedge F$ term in the Lagrangian of axion-electrodynamics. We find that magnetic fields larger than the observational lower bounds can be generated soon after recombination on scales of $1 {\rm{Mpc}}$.
Forward citations
Cited by 4 Pith papers
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Numerical Backreaction and Finite-Time Energy Transfer in Post-Recombination Magnetogenesis from Ultralight Dark Matter
Numerical simulations of post-recombination axion dark matter show that for dimensionless coupling α_eff ≳ 0.39, over half the dark-matter energy is transferred into gauge-field modes before back-reaction stops the resonance.
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A Non-Inflationary Axion and ALP Misalignment Mechanism
A thermally mediated, Planck-suppressed symmetry breaking potential can supply the initial axion misalignment that inflationary cosmology normally provides, allowing late-time coherent oscillations without inflation.
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Minimal Magnetogenesis: The Role of Inflationary Perturbations and ALPs, and Its Gravitational Wave Signatures
Inflationary curvature perturbations seed weak magnetic fields, and post-recombination axion oscillations amplify them to observed levels while sourcing detectable secondary gravitational waves.
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Parametric Resonance and Backreaction Effects in Magnetogenesis from Ultralight Dark Matter
A narrow parametric resonance channel exists in axion-DM magnetogenesis, but its claimed dominance at very small couplings is undermined by unchecked expansion damping.
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