Wright, D. J. ; De Cat, P. ; Pollard, K. R. ; Zima, W.

published in Communications in Asteroseismology, 157, pp. 383-384 (2008)

Abstract: The lack of well-identified modes is one of the major problems preventing an in-depth as- teroseismic study of gravity-mode (g-mode) main sequence pulsators. Since several of the currently available spectroscopic mode identification techniques have been developed for, or only extensively tested on pressure-mode pulsations, we started an investigation to improve them for the high radial order g-modes observed for slowly pulsating B (SPB) and γ Doradus (γ Dor) stars. A few high quality spectroscopic timeseries are being obtained for a selection of the most promising members of these groups with a large spread in projected rotational velocity that will serve as testbeds. These data will also enable us to study any observational relationship between the observed g-modes (degree l, azimuthal number m and/or pulsation amplitude) and the rotation of these non-radially pulsating stars.

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