https://doi.org/10.1051/epjconf/201716003013
On possible explanations of pulsations in Maia stars
1
Inytut Astronomiczny, Uniwersytet Wrocławski, ul. Kopernika 11, Wrocław, Poland
2
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716, Warsaw, Poland
⋆ e-mail: daszynska@astro.uni.wroc.pl
Published online: 27 October 2017
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.
© Owned by the authors, published by EDP Sciences, 2017
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (http://creativecommons.org/licenses/by/4.0/).
