Challenges in Inflationary Magnetogenesis: Constraints from Strong Coupling, Backreaction and the Schwinger Effect

Abstract

Models of inflationary magnetogenesis with a coupling to the electromagnetic action of the form $f^2{F}_{\mu \nu }{F}^{\mu \nu }$, are known to suffer from several problems. These include the strong coupling problem, the back reaction problem and also strong constraints due to Schwinger effect. We propose a model which resolves all these issues. In our model, the coupling function, $f$, grows during inflation and transits to a decaying phase post inflation. This evolutionary behaviour is chosen so as to avoid the problem of strong coupling. By assuming a suitable power law form of the coupling function, we can also neglect back reaction effects during inflation. To avoid back reaction post-inflation, we find that the reheating temperature is restricted to be below $\approx 1.7\times 10^4$ GeV. The magnetic energy spectrum is predicted to be non-helical and generically blue. The estimated present day magnetic field strength and the corresponding coherence length taking reheating at the QCD epoch(150 MeV) are $1.4\times 10^{-12}$ G and $6.1\times 10^{-4}$ Mpc, respectively. This is obtained after taking account of nonlinear processing over and above the flux freezing evolution after reheating. If we consider also the possibility of a non-helical inverse cascade, as indicated in direct numerical simulations, the coherence length and the magnetic field strength are even larger. In all cases mentioned above, the magnetic fields generated in our models satisfy the $\gamma$-ray bound below a certain reheating temperature.

13 pages, 4 figures, Published in PRD

References in corpus (9)

• On the Origin of Cosmic Magnetic Fields
• Generation of Large-Scale Magnetic Fields in Single-Field Inflation
• Magnetic fields from inflation?
• Nonhelical inverse transfer of a decaying turbulent magnetic field
• Schwinger Effect in 4D de Sitter Space and Constraints on Magnetogenesis in the Early Universe
• Classes of hydrodynamic and magnetohydrodynamic turbulent decay
• Inverse cascade of non-helical magnetic turbulence in a relativistic fluid
• Magnetic Fields from QCD Phase Transitions
• A scenario for inflationary magnetogenesis without strong coupling problem

Cited by in corpus (7)

• Early Cosmological Evolution of Primordial Electromagnetic Fields
• Seed magnetic fields in turbulent small-scale dynamos
• Schwinger Mechanism During Inflation
• Primordial Magnetogenesis in a Bouncing Universe
• Inflationary magnetogenesis with helical coupling
• Cosmological magnetic braking and the formation of high-redshift, super-massive black holes
• Astrophysics in Strong Electromagnetic Fields and Laboratory Astrophysics