  This paper presents the study of the interstellar medium toward beta CMa, a
disk sight-line known for its low neutral gas density. This study uses high and
medium resolution HST-GHRS spectra including lines from many species. The line
of sight to beta CMa (153 pc) is dominated by two ionized regions with a
velocity difference of 10 km/s. Their gas-phase abundances indicate that their
depletion is low, especially for the more ionized of the two clouds. Special
models of photoionization by the two EUV-excess stars beta CMa and epsilon CMa
would be needed for a detailed discussion of the ionizing mechanisms of the
clouds ; their ionization ratios are nevertheless roughly compatible with
collisional ionization at temperatures around 20 000 K, substantially higher
than the kinetic temperatures derived from the line widths. Their
characteristics suggest that the clouds may be in the process of cooling down
and recombining after having been shocked and ionized by some violent events,
possibly related to the Local Bubble formation.
