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In early-type Be stars, groups of nonradial pulsation (NRP) modes withnumerically related frequencies may be instrumental for the release of excessangular momentum through mass-ejection events. Difference and sum/harmonicfrequencies often form additional groups. The goal of this study is to find outwhether a similar frequency pattern occurs in the cooler third-magnitudeB7-8\,IIIe shell star $\nu$ Pup. Time-series analyses are performed of spacephotometry with BRITE-Constellation (2015, 2016/17, and 2017/18), SMEI(2003--011), and Hipparcos (1989-1993). Two IUE SWP and 27 optical echellespectra spanning 20 years were retrieved from various archives. The opticalspectra exhibit no anomalies or well-defined variabilities. A magnetic fieldwas not detected. All three photometry satellites recorded variability near0.656 c/d which is resolved into three features separated by ~0.0021 c/d. Firstharmonics form a second frequency group, also spaced by ~0.0021 c/d. Thefrequency spacing is very nearly but not exactly equidistant. Variability near0.0021 c/d was not detected. The long-term frequency stability could be used toderive meaningful constraints on the properties of a putative companion star.The IUE spectra do not reveal the presence of a hot subluminous secondary.$\nu$\,Pup is another Be star exhibiting an NRP variability pattern withlong-term constancy and underlining the importance of combination frequenciesand frequency groups. The star is a good target for efforts to identify aneffectively single Be star.

astronomy and astrophysics

Short-term variability and mass loss in Be stars IV. Two groups of  closely spaced, approximately equidistant frequencies in three decades of  space photometry of $\nu$ Puppis (B7-8 IIIe)