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Spectroscopic Analysis of BW Vulpeculae
A. Stankov1, M. Fridlund2, I. Ilyin3
1 Research and Scientific Support Department, ESA-ESTEC, SCI-SR, P.O. Box 229, 2200 AG Noordwijk, The Netherlands
2 Research and Scientific Support Department, ESA-ESTEC, SCI-SA, P.O. Box 229, 2200 AG Noordwijk, The Netherlands 3 Astronomy Division, P.O. Box 3000 FIN-90014 University of Oulu, Finnland
We present the results of the analysis of 40 echelle spectra of the
Last changed: 2002/Jun/18
©1996-2002 CAUP |
Cephei
star BW Vulpeculae. The data was obtained during two nights with the SOFIN spectrograph
at the Nordical Optical Observatory and covers a wavelength range from 4200 AA to
6600 AA. Comparing a synthetic spectrum calculated from a model atmosphere for this
star utilizing the program ATLAS9 by Kurucz, we determined the projected rotational
velocity, v sin i, to be 24 km/s. Then we performed detailed spectral line
identification and determined the formation depth of the lines. Furthermore,
we performed an abundance analysis for this star. From this analysis we find
that the following elements are overabundant in BW Vulpeculae: Si, Al, He, N,
Ne, Fe and Mg. Whereas O and S are underabundant. We also show the relation
between radial velocity and phase.