  The analysis of the BRITE oscillation spectrum of the main sequence early
B-type star $\nu$ Eridani is presented. Only models with the modified mean
opacity profile can account for the observed frequency ranges as well as for
the values of some individual frequencies. The number of the $\kappa$ modified
seismic models is constrained by the nonadiabatic parameter $f$, which is very
sensitive to the opacity changes in the subphotospheric layers where the
pulsations are driven. We present an example of the model that satisfies all
the above conditions. It seems that the OPLIB opacities are preferred over
those from the OPAL and OP projects. Moreover, we discuss additional
consequences of the opacity modification, namely, an enhancement of the
efficiency of convection in the Z-bump as well as an occurrence of close radial
modes which is a kind of avoided-crossing phenomenon common for nonradial modes
in standard main sequence models.
