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- W1975835253 abstract "Context.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 SMC is lower than , it constitutes a very suitable object to test these predictions." @default.
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- W1975835253 date "2008-01-02" @default.
- W1975835253 modified "2023-10-03" @default.
- W1975835253 title "Pulsating B and Be stars in the Small Magellanic Cloud" @default.
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- W1975835253 doi "https://doi.org/10.1051/0004-6361:20078754" @default.
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