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Searching for Spectral Line Variations in HgMn Stars
S. Turcotte1, C. Aerts2, P. Knoglinger3
1 Lawrence Livermore National Laboratory, L-413, P.O. Box 808,
Livermore, CA 94551, USA
2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B - 3001 Leuven, Belgium 3 Institute for Astronomy, University of Vienna, Turkenschanzstrasse 17, A-1180 Vienna, Austria
HgMn stars are chemically peculiar B stars that
are reputed as being some of the more constant stars known as no
strong evidence for variability has ever
been uncovered in any member of the class.
To this date, most of the searches for variability have
been made photometrically. An additional effort to discover or rule out variability
of these stars is motivated by theoretical expectations of pulsations
similar to those of SPB stars and by the possible discovery of star spots
suggested by earlier studies of a few HgMn stars. Progress in either of
these questions would provide essential information on the structure and
dynamics of these stars and by extension of cool B stars in general.
To this end, Echelle spectra taken with the Coralie spectrograph at La Silla of four HgMn
stars are used to search for line profile variability (LPV).
The four stars are
Last changed: 2002/Jun/25
©1996-2002 CAUP |
Phe (HD11753), 
Scl (HD221507), 41 Eri
(HD27376), and 
CMa (HD53244). All four are constant
photometrically within the current uncertainties.