Magnetization of the intergalactic medium by primeval galaxies

We review what has recently been learned from starburst-driven "superwinds, " galaxy-scale outflows, dwarf galaxy surveys, and evidence for early-unive rse merging scenarios. We apply this knowledge to simplified model populati ons of dwarf galaxies in the primeval galaxy era to demonstrate how a subst antial fraction of the intergalactic medium can be permeated with magnetic fields by dwarf galaxy outflow winds in the " volcanic early universe." Mec hanisms of both magnetic field regeneration and diffusion are discussed as they apply to galaxies at both primeval and later epochs of the universe. W e propose that, in the past, magnetic field strengths in outflow superbubbl es and halos were stronger than those now prevailing in the disks of curren t-epoch galaxies such as the Milky Way. We also show how subsequent acausal diffusion of magnetic fields (which we have not modeled) can propagate the fields over great distances in the universe within a Hubble time. We concl ude that dwarf galaxies can effectively seed the intergalactic medium with magnetic fields for a wide range of outflow and galaxy density parameters. If the first galaxies form at or before z similar to 10 in a "bottom-up" hi erarchical merging scenario, a substantial fraction of the intergalactic me dium will become permeated with a magnetic field at the present epoch. This intergalactic field seeding is largely accomplished by z similar to 6.