Large-scale magnetic fields in texture-seeded cosmological models

Details Large-scale magnetic fields in texture-seeded cosmological models Large-scale magnetic fields in texture-seeded cosmological models

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.287....1s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 287, Issue 1, pp. 1-9.

Astronomy and Astrophysics

Astronomy

12

Magnetic Fields, Cosmology: Miscellaneous, Large-Scale Structure Of Universe, Radio Continuum: General, Radio Lines: General

Scientific paper

After reviewing the problem of large-scale magnetic field generation, it is shown how the Harrison mechanism can generate magnetic fields on galactic scales or larger when protostructures have obtained angular momentum by the recombination epoch. In some models of large-scale structure formation there can be dynamically generated vorticity, or gravitational tidal torquing can cause the dark matter (DM) to acquire rms vorticity before the epoch of recombination. At recombination, the baryonic matter infalling in the DM potential wells acquires a net vorticity arising from dissipative effects in hydrodynamical shocks. For texture models, there is also some initial rms vorticity which contributes to the rms vorticity at recombination. An upper limit to the magnetic field thus generated by the Harrison mechanism in the context of the texture scenario of large-scale structure formation is calculated. Without re-ionization the seed magnetic field upper limit of 10^-22 G falls short of the value required by an exponential dynamo mechanism. If, as is likely in the texture scenario, the Universe was re-ionized at high redshift the resulting seed field is compatible with the dynamo mechanism.

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