6533b828fe1ef96bd1288cda

RESEARCH PRODUCT

Pulsating B and Be Stars in the Magellanic Clouds

Juan FabregatChristophe MartayanJuan Gutiérrez-sotoP. D. DiagoJ. Suso

subject

PhysicsOpacityAstrophysics::High Energy Astrophysical PhenomenaMetallicitySpectral domainAstrophysics::Cosmology and Extragalactic AstrophysicsAstrophysicsInstabilityLarge sampleStars13. Climate actionAstrophysics::Solar and Stellar AstrophysicsSmall Magellanic CloudLarge Magellanic CloudAstrophysics::Galaxy Astrophysics

description

Stellar pulsations in main-sequence B-type stars are driven by the κ-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 Z = 0. 002 for the Small Magellanic Cloud (SMC) and Z = 0. 007 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.

yearjournalcountryeditionlanguage
2010-01-01
https://doi.org/10.1007/978-3-642-11250-8_99