  Large scale strong magnetic fields in galaxies are generally thought to have
been generated by a mean field dynamo. In order to have generated the fields
observed, the dynamo would have had to have operated for a sufficiently long
period of time. However, magnetic fields of similar intensities and scales to
the one in our galaxy, are observed in high redshift galaxies, where a mean
field dynamo would not have had enough time to produce the observed fields.
Instead of a mean field dynamo, we study the emergence of strong large scale
magnetic fields in the first objects formed in the universe due to the action
or a turbulent, helical stochastic dynamo, for redshifts $5 \leq z \leq 10$.
Ambipolar drift plays an important role in this process due to the low level of
ionization of the gas, allowing a large scale stochastic dynamo to operate. We
take into account the uncertainties in the physics of high redshift objects by
examining a range of values for the parameters that characterize the turbulent
plasma. By numerically integrating the nonlinear evolution equations for the
magnetic field correlations, we show that for reasonable values of the
parameters in the time interval considered, fields can grow to high intensities
($\sim 10^{-6}$ G), with large coherence lengths ($\sim 2-6$ kpc), essentially
independent of the initial values of the magnetic field.
