2000MNRAS.318..341B

We present time-series spectroscopy of the rapidly oscillating Ap (roAp) star HR 3831. This star has a dominant pulsation period of 11.7min and a rotation period of 2.85d. We have analysed 1400 intermediate-resolution spectra of the wavelength region 6100-7100Å obtained over one week, using techniques similar to those we applied to another roAp star, α Cir.

We confirm that the Hα velocity amplitude of HR 3831 is modulated with rotation phase. Such a modulation was predicted by the oblique pulsator model, and rules out the spotted pulsator model. However, further analysis of Hα and other lines reveals rotational modulations that cannot easily be explained using the oblique pulsator model. In particular, the phase of the pulsation as measured by the width of the Hα line varies with height in the line.

The variation of the Hα bisector shows a very similar pattern to that observed in α Cir, which we have previously attributed to a radial node in the stellar atmosphere. However, the striking similarities between the two stars, despite the much shorter period of α Cir (6.8min), argues against this interpretation unless the structure of the atmosphere is somewhat different between the two stars. Alternatively, the bisector variation is a signature of the degree ℓ of the mode and not the overtone value n.

High-resolution studies of the metal lines in roAp stars are needed to understand fully the form of the pulsation in the atmosphere.