Other
Scientific paper
Aug 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248..214s&link_type=abstract
Astrophysical Journal, Part 1, vol. 248, Aug. 15, 1981, p. 214-221.
Other
5
Early Stars, Main Sequence Stars, Spectral Line Width, Stellar Oscillations, Stellar Spectra, B Stars, Balmer Series, O Stars, Stellar Models, Variable Stars
Scientific paper
High-resolution Reticon observations of the zero-age main-sequence star (ZAMS) υ Orionis over 1976-1979 show periodic line profile variations interpreted in terms of small-amplitude nonradial pulsations. Except for one interval in which a period of 23.52 hi was twice observed, υ Ori usually exhibits a period of ∼12.3 hr.
Viewed in the context of other line profile variable B stars (53 Per-type), υ Ori shows an average period length and a comparatively high period stability. In this last respect it resembles 10 Lac, another of the hotter members of the 53 Per group. The periods determined in υ Ori are sufficiently well known to state that period changes in 53 Per variables do not necessarily involve exact ratios of 2.
The most significant aspect of this study is that a ZAMS B star may pulsate nonradially. On theoretical grounds, it is argued that this fact makes the stellar core an unlikely site for the excitation of these oscillations.
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