Pulsating B and Be stars in the Magellanic Clouds
Abstract
Stellar pulsations in main-sequence B-type stars are driven by the -mechanism due to the Fe-group opacity bump. The current models do not predict the presence of instability strips in the B spectral domain at very low metallicities. As the metallicity of the Magellanic Clouds (MC) has been measured to be around for the Small Magellanic Cloud (SMC) and for the Large Magellanic Cloud (LMC), they constitute a very suitable objects to test these predictions. The aim of this work is to investigate the existence of B-type pulsators at low metallicities, searching for short-term periodic variability in a large sample of B and Be stars from the MC with accurately determined fundamental astrophysical parameters.
Keywords
Cite
@article{arxiv.0810.0166,
title = {Pulsating B and Be stars in the Magellanic Clouds},
author = {P. D. Diago and J. Gutiérrez-Soto and J. Fabregat and C. Martayan and J. Suso},
journal= {arXiv preprint arXiv:0810.0166},
year = {2008}
}
Comments
4 pages, 1 figure, contributed poster to the VIII Reuni\'on Cient\'ifica de la SEA 2008, Santander 7-11 July 2008 (v2 corrects a misprint in title)