  A linear stability analysis of a multi-component and magnetized Galactic disk
model is presented. The disk model uses the observed stratifications for the
gas density and gravitational acceleration at the solar neighborhood and, in
this sense, it can be called a realistic model. The distribution of the total
gas pressure is defined by these observed stratifications, and the gaseous disk
is assumed isothermal. The initial magnetic field is taken parallel to the
disk, with a midplane value of 5 $\mu$G, and its stratification along the
z-axis is derived from the condition of magnetohydrostatic equilibrium in an
isothermal atmosphere. The resulting isothermal sound speed is $\sim 8.4$ km
s$^{-1}$, similar to the velocity dispersion of the main gas components within
1.5 kpc from midplane. The thermal-to-magnetic pressure ratio decreases with
$[z]$ and the warm model is Parker unstable. The dispersion relations show that
the fastest growing mode has a wavelength of about 3 kpc, for both symmetric
and antisymmetric perturbations, and the corresponding growth time scales are
of about $3\times 10^7$ years. The structure of the final equilibrium stage is
also derived, and we find that the midplane antisymmetric (MA) mode gathers
more gas in the magnetic valleys. The resulting MA gas condensations have
larger densities, and the column density enhancement is a factor of about 3
larger than the value of the initial stage. The unstable wavelengths and growth
times for the multi-component disk model are substantially larger than those of
a thin disk model, and some of the implications of these results are discussed.
