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Magnetic Field Generation in Protogalactic Halos

Published online by Cambridge University Press:  19 July 2016

Ralph E. Pudritz
Ralph E. Pudritz*
Affiliation:
Dept. of Physics, McMaster University, Hamilton, ON L8S 4M1

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It has become quite clear that dynamically significant magnetic fields of order 10−6 Gauss are present in galactic halos (Perry, these Proceedings) at redshifts up to z ≥ 2. Comparable fields have been detected on cluster and even on supercluster scales (Giovannini, these Proceedings). The existence of such high fields is surprising because it is highly unlikely that primeval magnetic fields could have been much stronger than 10–18 Gauss. These observations require that there be an epoch of very vigorous dynamo action that can amplify this seed primordial field up to the observed values. Since strong fields are already in place by redshifts of z ≃ 2, this amplification process must operate very quickly. This argues against the idea that such fields could be generated on huge intercluster scales since the dynamical times are far too long. A much more promising site for the dynamo process is in the dark matter halos of young galaxies during the epoch of galaxy formation. The fundamental point is that vigorous dynamo action can take place in shocks that are expected to occur throughout the dark matter potential wells of protogalaxies (Pudritz and Silk 1989 (≡ PS), Pudritz 1989).

Type
10. Magnetic Fields at High Redshifts and in the Early Universe
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 519 - 526
Copyright
Copyright © Kluwer 1990 

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