SEISMOLOGY OF SOUTHERN Be STARS EDUARDO JANOT-PACHECO and NELSON VANI LEISTER Depto. Astronomie, IAG-USP, Brazil 1. The survey: search for rapid variability in Be stars We have started in 1990 a search for moving bumps in the Hel 667.8 nm of mainly southern, bright Be stars. The objects of our sample have been selected on the basis of photometric variability (Cuypers et al., 1989). High resolution ( R > 30,000), high signal-to-noise ratio ( S / R > 300) spec- troscopic observations have been performed at the brazilian Laboratorio Nacional de Astrofisica with a CCD camera attached to the coud spectro- graph of the 1.60 m telescope (e.g. Table I). Several hundred spectra have been taken during the last three years. Photometric observations simulta- neous with spectroscopy were made on the same site in July 1992 with a two-channel photometer (Stromgren 6 filter) and a CCD camera (Johnson filter) installed at two 0.60 m telescopes. The idea is try to disentangle the controversy between NRP and RM models with the help of simultaneous spectroscopy and photometry. TABLE I Some Be stars observed at L.N.A. Star Epoch Type of Observation Remarks a Eri 1990-93 Spectroscopy / = |m| ~ 10 1990-93 Photometry 1993 CCD Eri 1990 Spectroscopy bumps? 1993 Photometry 1993 CCD ; Cen 1990-93 Spectroscopy / = \m\ ~ 14 C Oph 1990-93 Spectroscopy / = \m\ ~ 7 2 Some results Moving subfeatures are seen in ~ 50% of the stars in our sample, a Eri is discussed elsewhere in this meeting (Leister et al., 1993a this volume). 104 L. A. Balona et al (eds.), Pulsation, Rotation and Mass Loss in Early-Type Stars, 104-105. 19941AU. Printed in the Netherlands. available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900214630 Downloaded from https://www.cambridge.org/core. IP address: 207.241.231.81, on 25 Jul 2018 at 02:38:06, subject to the Cambridge Core terms of use,