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In most of the literature on evolution of cosmological magnetic fields, it isfound that large-scale magnetic fields evolve as $B^{2}\propto a^{-4}$(adiabatic magnetic decay) where $a$ is the cosmological scale factor and $B$is the cosmological magnetic field. This rapid decay has been considered as themain obstacle against magnetic fields produced during the inflationary epochfrom surviving until today and seeding the observed fields. However, recentreports of first ever detection of intergalactic fields, with strengths around$10^{-6}G$ are a mystery [1-4]. One possible explanation is that large-scalemagnetic fields could have been superadiabatically amplified in theirevolutionary history. Superadiabatic amplification may mean that there is anactual increase in the strength of the magnetic field or that magneticdecay-rates are slower than the standard adiabatic magnetic decay rate [5] .This can be demonstrated if we use the generalised cosmological Ohm's law andboth standard and modified Maxwell field equations; this is the goal of thisstudy.

Post inflationary evolution of inflation-produced, large-scale magnetic  fields using a generalised cosmological Ohm's law and both standard and  modified Maxwell's equations