SIMBAD references

We report a time-series analysis of the O4 I(n)fp star ζPup, based on optical photometry obtained with the SMEI (Solar Mass Ejection Imager) instrument on the Coriolis satellite, 2003-2006. A single astrophysical signal is found, with P = 1.780938±0.000093 d and a mean semi-amplitude of 6.9±0.3 mmag. There is no evidence for persistent coherent signals with semi-amplitudes in excess of ∼ 2 mmag on any of the time-scales previously reported in the literature. In particular, there is no evidence for a signature of the proposed rotation period, ∼ 5.1 d; ζ Pup is therefore probably not an oblique magnetic rotator. The 1.8-d signal varies in amplitude by a factor ∼ 2 on time-scales of 10-100d (and probably by more on longer time-scales), and exhibits modest excursions in phase, but there is no evidence for systematic changes in period over the 1000-d span of our observations. Rotational modulation and stellar-wind variability appear to be unlikely candidates for the underlying mechanism; we suggest that the physical origin of the signal may be pulsation associated with low-ℓ oscillatory convection modes.