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 ν Puppis (B7-8 IIIe)⋆,⋆⋆,⋆⋆⋆
European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Karl-Schwarzschild-Str. 2, 85748, Garching
2 Astronomical Institute, Wrocław University, Kopernika 11, Wrocław 51-622, Poland
3 European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Santiago 19, Casilla 19001, Chile
4 Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, GA 30302-5060, Atlanta PO Box 5060, USA
5 Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, Warsaw 00-716, Poland
6 Observatório Nacional, Rua General José Cristino 77, São Cristóvão, Rio de Janeiro 20921-400, Brazil
7 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Cidade Universitária, Rua do Matão 1226, São Paulo, SP 05508-900, Brazil
8 Institut für Kommunikationsnetze und Satellitenkommunikation, Technical University Graz, Inffeldgasse 12, Graz 8010, Austria
9 Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, CP 6128, Succ. Centre-Ville, Montréal Québec H3C 3J7, Canada
10 AAVSO Headquarters, 49 Bay State Rd., Cambridge, MA 02138, USA
11 Department of Astronomy and Astrophysics, University of Toronto, 50 St. George St., Toronto, Ontario M5S 3H4, Canada
12 Department of Physics and Space Science, Royal Military College of Canada, Stn Forces, Ontario K7K 7B4, , Kingston PO Box 17000, Canada
13 Institute of Astrophysics, University of Vienna, Universitätsring 1, Vienna 1010, Austria
14 Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstrasse 25, Innsbruck 6020, Austria
Accepted: 13 October 2018
Context. In early-type Be stars, groups of nonradial pulsation (NRP) modes with numerically related frequencies may be instrumental for the release of excess angular momentum through mass-ejection events. Difference and sum/harmonic frequencies often form additional groups.
Aims. The purpose of this study is to find out whether a similar frequency pattern occurs in the cooler third-magnitude B7-8 IIIe shell star ν Pup.
Methods. Time-series analyses were performed of space photometry with BRITE-Constellation (2015, 2016/17, and 2017/18), SMEI (2003–2011), and HIPPARCOS (1989–1993). Two IUE SWP and 27 optical echelle spectra spanning 20 years were retrieved from various archives.
Results. The optical spectra exhibit no anomalies or well-defined variabilities. A magnetic field was not detected. All three photometry satellites recorded variability near 0.656 c/d which is resolved into three features separated by ∼0.0021 c/d. Their first harmonics and two combination frequencies form a second group, whose features are similarly spaced by 0.0021 c/d. The frequency spacing is very nearly but not exactly equidistant. Variability near 0.0021 c/d was not detected. The long-term frequency stability could be used to derive meaningful constraints on the properties of a putative companion star. The IUE spectra do not reveal the presence of a hot subluminous secondary.
Conclusions. ν Pup is another Be star exhibiting an NRP variability pattern with long-term constancy and underlining the importance of combination frequencies and frequency groups. This star is a good target for efforts to identify an effectively single Be star.
Key words: asteroseismology / stars: emission-line, Be / stars: mass-loss / techniques: photometric / stars: rotation
Based in part on data collected by the BRITE-Constellation satellite mission, built, launched and operated thanks to support from the Austrian Aeronautics and Space Agency and the University of Vienna, the Canadian Space Agency (CSA), and the Foundation for Polish Science & Technology (FNiTP MNiSW) and National Science Centre (NCN).
Based in part on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 074.D-0240.
Light curve data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/620/A145
© ESO 2018