section 6. The results of section 5 and 6, suggests a useful visualisation of the spatial distribution of the small-scale dynamo generated field (cf. Zeldovich et. al, 1983). We argue that in the galactic context, the magnetic field generated by small scale dynamo action, concentrates into thin (perhaps ropy) structures. One of the aims of our work here is to lay a framework for a companion paper (Subramanian, 1997 : Paper I). In Paper I we have built upon the results obtained in sections 5 and 6, to discuss in detail how the small-scale dynamo may saturate in the galactic context, in a manner which preserves large-scale dynamo action.

Section 7 concentrates on the kinematic evolution of the helical component of the magnetic correlations. The study of helical magnetic correlations has been mostly neglected in the literature, since they do not drastically affect the small-scale dynamo. However the evolution of current helicity is important in determining the back reaction of small-scale fields on the $\alpha$-effect in the standard dynamo equation (cf. Pouquet [*et al.*]{} 1976, Zeldovich [*et al.*]{} 1983, Gruzinov and Diamond 1994, Bhattacharjee and Yuan 1995). Numerical simulations by Tao [*et al.*]{}, 1993 indicated that the alpha effect is 