Pulsating B and Be stars in the Magellanic Clouds
  Stellar pulsations in main-sequence B-type stars are driven by the $\kappa$-mechanism due to the Fe-group opacity bump. The current models do not predict the presence of instability strips in the B spectral domain at very low metallicities. As the metallicity of the Magellanic Clouds has been measured to be around $Z=0.002$ for the SMC and $Z=0.007$ for the LMC, they constitute a very suitable objects to test these predictions. 
P.D. Diago, J. Guti\'errez-Soto, J. Fabregat, C. Martayan and J. Suso