Abstract
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 $\delta$ 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.
Highlights
Pulsating variables between the instability strips of δ Scuti and Slowly Pulsating B-type (SPB) stars have been suggested many years ago by Struve [1]
We found that by increasing the mean opacity at the depth log T = 5.1 in a M = 2.5 M model, it is possible to get the instability in the observed frequency range for modes with ≥ 2
Fast rotating stars seen equator-on can account for pulsations of the Maia type
Summary
Pulsating variables between the instability strips of δ Scuti and Slowly Pulsating B-type (SPB) stars have been suggested many years ago by Struve [1]. New scenario, we modify the opacity profile in order to excite pulsational modes in the required frequency range in the rotating models with masses below e-mail: daszynska@astro.uni.wroc.pl The last hypothesis demands the modifications of the opacity profile and higher degree modes (up to 6-8) and works for both, low and fast rotating stars of
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