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Survey for line-profile variability in early-B type
main-sequence stars
J.H. Telting1, K. Uytterhoeven2,3, and I. Ilyin4
1 Nordic Optical Telescope, Apartado de Correos 474, 38700 Santa
Cruz de La Palma, Spain
2 Instituut voor Sterrenkunde, KULeuven, Celestijnenlaan 200B, 3001
Leuven, Belgium
3 Mercator Telescope, Apartado de Correos 565, 38700 Santa Cruz de
La Palma, Spain
4 Astronomy Division, P.O. box 3000, 90014 University of Oulu, Finland
We present the results of our high-resolution spectroscopic survey
of line-profile variations in stars with similar spectral types as
 Cephei stars. In this paper we focus on the northern
hemisphere, to complement the southern survey of Schrijvers et al.
2002 (IAU Coll. 185, ASP Conf. Series 259, p. 204).
In three observing runs between November 2001 and March 2002 we
obtained spectra of 38 main-sequence stars with the SOFIN spectrograph
on the Nordic Optical Telescope at La Palma. We took more than 100
spectra all together, centered on the SiIII 4552 and 4567 lines, with
S/N typically better than 350. The spectral resolution used was
between R=50000 (high v sin i stars) and R=65000 (low v sin i
stars), which means we can resolve pulsational bump patterns for stars
with v sin i larger than about 30 km/s.
For 33 % of our targets that have v sin i higher than 35 km/s, we
find clear evidence for the existence of pulsations, in the form of
bump patterns in the line profiles or in the form of line shifts. For
another 24 % we need more data to confirm suspected bump patterns.
This indicates that many early-B type stars may be pulsationally
excited.
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Last changed: 2002/Jun/25
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