lane, seen in the B image, superimposed on the gap. The probable action of a fast wind arising from ob33wr2 is evident from a small cavity (blown?) in the wall this shell, south-east of the star. An arc is seen surrounding ob10wr1 (see Figure 1d) perhaps being driven into ob10 by the expansion of this Group Ib shell. Finally, the potential action of a WR wind can be seen for the case of the Group IIa star MS17 (see Figure 2a), where it has apparently disrupted the wall of a diamond shaped shell, in which it is embedded.

Obtaining detailed kinematics (in both the ionized and neutral gas) of these interacting shells, and the gas effected by WR winds, may prove extremely useful in understanding the dynamical evolution of shell structures in the ISM of galaxies. Further, in addition to spectroscopy, narrow-band imaging, in lines such as \[\]$\lambda$5007 or \[\]$\lambda$6300, may prove useful in detecting shock fronts in a wind-ISM interaction region. Will shells merge to become larger single structures? What role do WR winds play in enlarging pre-existing shell structures? Are the shells, presented in this paper, the evolutionary precursors of shells (or supershells). What role do WR stars 