Pulsating B and Be stars in the Magellanic Clouds

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dc.creatorDiago, P. D.
dc.creatorGutiérrez-Soto, J.
dc.creatorFabregat, J.
dc.creatorMartayan, C.
dc.creatorSuso, J.
dc.date2008-09-15
dc.date2008-10-02
dc.date.accessioned2026-07-07T10:06:33Z
dc.date.available2026-07-07T10:06:33Z
dc.descriptionStellar 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 has been measured to be around $Z=0.002$ for the SMC and $Z=0.007$ for the LMC, they constitute a very suitable objects to test these predictions.
dc.description2 pages, 1 figure, contributed poster to the Proceedings of the Wroclaw HELAS Workshop, 2008 - Submitted to Communications in Asteroseismology
dc.identifierhttps://arxiv.org/abs/0809.2481
dc.identifierhttp://arxiv.org/abs/0809.2481
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/170365
dc.subjectAstrophysics
dc.titlePulsating B and Be stars in the Magellanic Clouds
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