Serious questions concerning our knowledge of stellar structure and evolution can be addressed through the asteroseismology of hot stars in the LMC and SMC. There is an apparent discrepancy between the theoretical prediction of pulsational instability in B stars and what w observe in nature. This discrepancy appears to relate to the way the metal content of hot stars affects their internal structure. The LMC and SMC are ideal testing grounds for our theories. A long-term project to study this problem at Sutherland in South Africa will be reviewed.