More on pulsating B-type stars in the Magellanic Clouds

TL;DR

This study investigates B-type pulsators in the Magellanic Clouds, revealing a significant number of pulsators at low metallicity that challenge existing theoretical models and mapping their instability regions.

Contribution

It provides the first large-scale analysis of B-type pulsators in low-metallicity environments, highlighting discrepancies with current pulsation theories.

Findings

Detection of beta Cephei and SPB-like pulsators at low metallicity

Mapping of observational instability regions in the HR diagram

Comparison showing conflicts with existing pulsation models

Abstract

We present here the results of our research for B-type pulsators in low metallicity environments, searching for short-term periodic variability in a large sample of B and Be stars in the Magellanic Clouds (MC), for which the fundamental astrophysical parameters were accurately determined. A significant number of beta Cephei and SPB-like pulsators at low-metallicity have been detected, conflicting with the current theoretical models of pulsation. In addition, we have placed these pulsating stars in the HR diagram mapping the observational instability regions for the MC metallicities. The large sample of B and Be stars analysed allows 5Aus to make a reliable statistics of the pulsating B-type stars in the MC. Finally, we have made a comparison between pulsational theory and observations in low metallicity environments.