  To contribute to the understanding of the magnetic field's influence on the
segregation of CNM in the solar neighbourhood we analyse MHD simulations which
include the main physical characteristics of the local neutral atomic ISM. The
simulations have a continuous solenoidal Fourier forcing in a periodic box of
100 pc per side and an initial uniform magnetic field ($\vec{B_0}$) with
intensities ranging between $\sim 0.4$ $\mu$G and $\sim 8$ $\mu$G. Our main
results are: i) the CNM mass fraction diminishes with the increase in magnetic
field intensity. ii) There is a preferred alignment between CNM structures and
$\vec{B}$ in all our $B_0$ range but the preference weakens as $B_{0}$
increases. It is worth noticing that this preference is also present in
two-dimensional projections making an extreme angle ($0$ or $\pi / 2$) with
respect to $\vec{B_0}$ and it is only lost for the strongest magnetic field
when the angle of projection is perpendicular to $\vec{B_0}$. iii) The
aforementioned results are prevalent despite the inclusion of self-gravity in
our continuously forced simulations with a mean density similar to the average
value of the solar neighbourhood. iv) Given a fixed $B_0$ and slightly higher
mean densities, up to double, the effects of self-gravity are still not
qualitatively significant.
