Abstract
Aims. Our goal is to test the newly developed OPLIB opacity tables from Los Alamos National Laboratory and check their influence on the pulsation properties of B-type stars.Methods. We calculated models using MESA and Dziembowski codes for stellar evolution and linear, nonadiabatic pulsations, respectively. We derived the instability domains of β Cephei and SPB-types for different opacity tables OPLIB, OP, and OPAL.Results. The new OPLIB opacities have the highest Rosseland mean opacity coefficient near the so-called Z -bump. Therefore, the OPLIB instability domains are wider than in the case of OP and OPAL data.
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