  We study the structure of shocks in clumpy media, using a multifluid
formalism. As expected, shocks broaden as they weaken: for sufficiently weak
shocks, no viscous subshock appears in the structure. This has significant
implications for the survival of dense clouds in regions overrun by shocks in a
wide range of astrophysical circumstances, from planetary nebulae to the nuclei
of starburst galaxies.
