Issue |
A&A
Volume 368, Number 1, March II 2001
|
|
---|---|---|
Page(s) | 160 - 174 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20000409 | |
Published online | 15 March 2001 |
BCD spectrophotometry of stars with the B[e] phenomenon *,**
I. Fundamental parameters
1
Facultad de Ciencias Astronómicas y Geofísicas, Universidad de La Plata, Paseo del Bosque S/N, 1900 La Plata, Argentina
2
Institut d'Astrophysique de Paris, CNRS, 98bis Bd. Arago, 75014 Paris, France
Corresponding author: J. Zorec, zorec@iap.fr
Received:
3
October
2000
Accepted:
29
November
2000
Low resolution spectra in the Åwavelength
range of 23 stars with the B[e] phenomenon are presented. Spectral
classification of 15 program stars was performed using the BCD
spectrophotometric system, based on the study of the Balmer discontinuity,
which is independent of interstellar and circumstellar dust extinctions and of
circumstellar gas emissions and/or absorptions. From calibrations of the
BCD parameters we determined the (
of the studied stars. For stars where this method could not be applied,
we tried to estimate the temperature of the central star by using the Balmer
and He i emission lines and/or their visible energy distribution. The
colour temperature and the temperatures obtained from the study of Balmer and
He i lines are consistent with each other. The new results are compared
with those obtained previously by other authors and discussed for each star
individually. For some stars, differences between the effective temperatures
derived using the BCD classification system and those obtained elsewhere,
based on photometric or spectroscopic analysis, imply spectral-type
classification disagreements ranging from 2-3 up to 6 B sub-spectral types.
The fundamental parameters of AS 119, CD-24°5721, Hen2-91, HD 316375
and BD-11°4747 were determined for the first time. A simple method was
introduced to calculate total (interstellar+circumstellar) dust extinction
towards the studied stars. For HD 53179, which is a double stellar system, and
for HD 45677 and HD 50138, which are suspected to be binaries, we predicted the
characteristics of the components that are consistent with the observed
parameters. However, the possible binarity of HD 45677 and HD
50138 still needs to be confirmed spectroscopically.
Key words: stars: emission-line, B[e] / stars: fundamental parameters / stars: evolution
© ESO, 2001
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