Abstract
SIGMA Orionis E, the first He-rich B star discovered1,2, was recently found3,4 to have an extremely broad (∼1,800 km s−1), rapidly varying Hα-emission feature. From independent spectroscopic, spectrophotometric, and photometric observations on 4 consecutive nights in December 1974, we have shown4 that it is a variable, with P ≃ 1.19 d; however, incomplete phase coverage in those data, as well as uncertainty about the nature of the periodicity, has hampered the development of a model to account for the wealth of observed phenomena. Here we briefly communicate results of new continuous uvbyβ photometry carried out during the 11 consecutive nights December 28, 1975–January 7, 1976 (UT), together with some possible interpretations.
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