Spectroscopic variabilities in λ Pavonis
Universidade Federal de São Paulo, Depto. Ciências Exatas e da
Terra, Rua Prof. Artur Riedel, 275,
Jd. Eldorado, CEP 09972-270, Diadema
2 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, CEP 05508-900 São Paulo, SP, Brazil
3 Instituto de Física, Universidade de São Paulo, Cidade Universitária, CEP 05508-900 São Paulo, SP, Brazil
Accepted: 14 July 2011
Aims. We investigate the time-varying patterns in line profiles, V/R, and radial velocity of the Be star HD 173948 (λ Pavonis).
Methods. Time series analyses of radial velocity, V/R, and line profiles of He i, Fe ii, and Si ii were performed with the Cleanest algorithm. An estimate of the stellar rotation frequency was derived from the stellar mass and radius in the Roche limit by adopting an aspect angle i derived from the fittings of non-LTE model spectra affected by rotation. The projected rotation velocity, necessary as input for the spectral synthesis procedure, was evaluated from the Fourier transform of the rotation profiles of all neutral helium lines in the optical range.
Results. Emission episodes in Balmer and He i lines, as well as V/R cyclic variations, are reported for spectra observed in year 1999, followed by a relatively quiescent phase (2000) and then again a new active epoch (2001). From time series analyses of line profiles, radial velocities, and V/R ratios, four signals with high confidence levels are detected: ν1 = 0.17 ± 0.02, ν2 = 0.49 ± 0.05, ν3 = 0.82 ± 0.03, and ν4 = 1.63 ± 0.04 c/d. We interpret ν4 as a non-radial pulsation g-mode, ν3 as a signal related to the orbital timescale of ejected material, which is near the theoretical rotation frequency 0.81 c/d inferred from the fitting of the models taken into account for gravity darkening. The signals ν1 and ν2 are viewed as aliases of ν3 and ν4.
Key words: stars: oscillations / stars: fundamental parameters / stars: emission-line, Be / stars: individual:λPavonis
© ESO, 2011