Pulsating B and Be stars in the Magellanic Clouds
| dc.creator | Diago, P. D. | |
| dc.creator | Gutiérrez-Soto, J. | |
| dc.creator | Fabregat, J. | |
| dc.creator | Martayan, C. | |
| dc.creator | Suso, J. | |
| dc.date | 2008-10-01 | |
| dc.date | 2008-10-02 | |
| dc.date.accessioned | 2026-07-07T10:06:41Z | |
| dc.date.available | 2026-07-07T10:06:41Z | |
| dc.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. | |
| dc.description | 4 pages, 1 figure, contributed poster to the VIII Reunión Científica de la SEA 2008, Santander 7-11 July 2008 (v2 corrects a misprint in title) | |
| dc.identifier | https://arxiv.org/abs/0810.0166 | |
| dc.identifier | http://arxiv.org/abs/0810.0166 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/170408 | |
| dc.subject | Astrophysics | |
| dc.title | Pulsating B and Be stars in the Magellanic Clouds | |
| dc.type | text |