Volume 415, Number 2, February IV 2004
|Page(s)||L13 - L16|
|Published online||11 February 2004|
Letter to the Editor
No magnetic field variation with pulsation phase in the roAp star γ Equulei
Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria
2 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 109017 Moscow, Russia
3 Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden
Corresponding author: O. Kochukhov, firstname.lastname@example.org
Accepted: 5 January 2004
We present an analysis of 210 high-resolution time-resolved spectropolarimetric observations of the roAp star γ Equ obtained over three nights in August and September 2003. Radial velocity variations due to p-mode non-radial pulsations are clearly detected in the lines of rare-earth elements, in particular , and . In contrast, we find absolutely no evidence for the variation of the mean longitudinal magnetic field over the pulsation period in γ Equ at the level of 110–240 G which was recently reported by Leone & Kurtz ([CITE]). Our investigation of the variability of circularly polarized profiles of 13 lines demonstrates that, at the 3σ confidence level, no magnetic field variation with an amplitude above ≈ G was present in γ Equ during our monitoring of this star.
Key words: stars: atmospheres / stars: chemically peculiar / stars: individual: γ Equ / stars: magnetic fields / stars: oscillations
© ESO, 2004
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