  Hydrostatic equilibrium of the multiphase interstellar medium in the solar
vicinity is reconsidered, with the regular and turbulent magnetic fields
treated separately. The regular magnetic field strength required to support the
gas is consistent with independent estimates provided energy equipartition is
maintained between turbulence and random magnetic fields. Our results indicate
that a midplane value of $B_{0}=4\mkG$ for the regular magnetic field near the
Sun leads to more attractive models than $B_{0}=2\mkG$. The vertical profiles
of both the regular and random magnetic fields contain disc and halo components
whose parameters we have determined. The layer at $1\la|z|\la4\kpc$ can be
overpressured and an outflow at a speed of about $50\kms$ may occur there,
presumably associated with a Galactic fountain flow, if $B_{0}\simeq 2\mkG$. We
show that hydrostatic equilibrium in a warped disc must produce asymmetric
density distributions in $z$, in rough agreement with \HI observations in the
outer Galaxy. This asymmetry may be a useful diagnostic of the details of the
warping mechanism in the Milky Way and other galaxies. We find indications that
gas and magnetic field pressures are different above and below the warped
midplane in the outer Galaxy and quantify the difference in terms of turbulent
velocity and/or magnetic field strength.
