  Two dimensional calculations of the evolution of remnants generated by the
strong mechanical energy deposited by stellar clusters in dwarf galaxies (M \si
$10^9 - 10^{10}$ \msun) are presented. The evolution is followed for times
longer than both the blowout time and the presumed span of energy injection
generated by a coeval massive stellar cluster. The remnants are shown to end up
wrapping around the central region of the host galaxy, while growing to
kpc-scale dimensions. Properties of the remnants such as luminosity, size,
swept up mass, and expansion speed are given as a function of time for all
calculated cases. The final fate of the swept-up galactic gas and of the matter
processed by the central starburst is shown to be highly-dependent on the
properties of the low density galactic halo. Superbubbles powered by star
clusters, with properties similar to those inferred from the observations, slow
down in the presence of an extended halo to expansion speeds smaller than the
host galaxy escape velocity. Values of the critical luminosity required for the
superbubbles to reach the edge of the galaxies with a speed comparable to the
escape speed are derived analytically and numerically. The critical
luminosities are larger than those in the detected sources and thus, the
superbubbles in amorphous dwarf galaxies must have already undergone blowout
and are presently evolving into an extended low density halo. This will inhibit
the loss of the swept-up and processed matter from the galaxy.
