  In paper I, we obtained an equation for the evolution of density
inhomogeneities in a radiation dominated universe when they are affected by
magnetic fields. In this second paper we apply this equation to the case in
which the subjacent magnetic configuration is a flux tube. For scales of the
order of 1 Mpc or less the differential equation is elliptical. To solve it, we
have used the numerical method based on "Simultaneous Over Relaxation", SOR,
with Chebyshev acceleration and we have treated the problem as a boundary value
problem, which restricts the prediction ability of the integration. For
large-scale flux tubes, much larger than 1 Mpc, the equation can be
analytically integrated and no assumption about the final shape or magnitude of
the inhomogeneity is required. In both cases we obtain an evolution which does
not differ very much from linear in time. The inhomogeneity in the density
becomes filamentary. Large scale structures ($\ge$ 10 Mpc) are probably
unaffected by damping, non-linear and amplification mechanisms after Equality,
so that this model provides a tool to interpret the present observed large
scale structure.
  Filaments are very frequently found in the large-scale structure in the
Universe. It is suggested here that they could arise from primordial magnetic
flux tubes, thus providing an alternative hypothesis for its interpretation; in
particular we consider the case of the Coma-A1367 supercluster, where the
magnetic field is known to be high.
