On possible explanations of pulsations in Maia stars

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.

proceedings of the Joint TASC2 - KASC9 Workshop - SPACEINN - HELAS8 Conference "Seismology of the Sun and the Distant Stars 2016", to be published by the EPJ Web of Conferences

References in corpus (4)

• A New Generation of Los Alamos Opacity Tables
• Pulsation frequency distribution in Delta Scuti stars
• The puzzling new class of variable stars in NGC 3766 : old friend pulsators?
• The hot Gamma-Doradus and Maia stars

Cited by in corpus (2)

• Highlights of Discoveries for $\delta$ Scuti Variable Stars From the Kepler Era
• Spots and flares in hot main sequence stars