Complex asteroseismology of theβCep/slowly pulsating B-type pulsatorνEridani: constraints on opacities

We undertake another attempt towards the seismic modelling of the most intensively studied main-sequence early B spectral type pulsator, ν Eridani. Our analysis is extended by a requirement of fitting not only pulsational frequencies but also the complex amplitude of the bolometric flux variation, f, related to each mode frequency. This approach, termed complex asteroseismology, provides a unique test of stellar parameters, atmospheres and opacities. In particular, the concordance of the empirical and theoretical values of f we obtained for the high-order g mode offers a new insight into seismic studies of main-sequence hybrid pulsators. The most intriguing and challenging result is that, whereas an agreement of the theoretical and empirical values of f for the radial mode can be achieved only with the OPAL data, a preference for the OP tables is obtained from the analysis of the high-order gravity mode.