On possible explanations of pulsations in Maia stars

The long-time photometric surveys in a few young open clusters allowed to identify the light variability in stars located on the HR diagram between the well defined δ Scuti variables and Slowly Pulsating B-type stars. Several objects of this type were suggested also from the analysis of the Kepler data. Assuming the pulsational origin of this variability, we try to explain the observed frequencies with pulsational models involving rotation and/or modification of the mean opacity profile

On possible explanations of pulsations in Maia stars

The long-time photometric surveys in a few young open clusters allowed to identify the light variability in stars located on the HR diagram between the well defined δ Scuti variables and Slowly Pulsating B-type stars. Several objects of this type were suggested also from the analysis of the Kepler data. Assuming the pulsational origin of this variability, we try to explain the observed frequencies with pulsational models involving rotation and/or modification of the mean opacity profile

Inference for stellar opacities from seismic studies of the hybrid β Cep/SPB pulsators

We present a comprehensive seismic study of the three pulsating stars of β Cep/SPB type: v Eridani, 12 Lacertae and γ Pegasi. Models with the modified mean opacity profile are constructed in order to account for both the observed frequency range and the values of some individual frequencies. To decrease the number of possible solutions, we make use of the non-adiabatic parameter f, whose value is very sensitive to subphotospheric layers where pulsations are driven. This complex seismic modelling shows the need for a significant modification of the opacity profile

Inference for stellar opacities from seismic studies of the hybrid β Cep/SPB pulsators

We present a comprehensive seismic study of the three pulsating stars of β Cep/SPB type: v Eridani, 12 Lacertae and γ Pegasi. Models with the modified mean opacity profile are constructed in order to account for both the observed frequency range and the values of some individual frequencies. To decrease the number of possible solutions, we make use of the non-adiabatic parameter f, whose value is very sensitive to subphotospheric layers where pulsations are driven. This complex seismic modelling shows the need for a significant modification of the opacity profile