Issue |
A&A
Volume 386, Number 3, May II 2002
|
|
---|---|---|
Page(s) | 1019 - 1027 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20020349 | |
Published online | 15 May 2002 |
An analysis of STIS HST UV spectra of M 33 early B supergiants*
1
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
2
Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, 38071 La Laguna, Spain
3
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA
4
Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany
Corresponding author: M. A. Urbaneja, maup@ll.iac.es
Received:
7
February
2002
Accepted:
4
March
2002
We present terminal velocities of M 33 B-supergiants, obtained
from STIS HST spectra
as part of our programme to investigate the Wind Momentum –
Luminosity Relationship (WLR) in the Local Group.
Terminal velocities are derived from their ,
, and
resonance lines in UV spectra. Comparing with
IUE spectra of Galactic B-supergiants we found evidence
of low metallicity in three of our objects.
The terminal velocities are consistent with the corresponding values of Galactic
stars, except for B-133. For this
star we find a very large
and a red
component deeper than the blue one, that might be an indication
of binarity. The average ratio
between terminal and turbulent wind velocities is 0.25,
well above the value found for Galactic stars.
Key words: stars: atmospheres / stars: early-types / stars: supergiants / stars: fundamental parameters / stars: winds, outflows / galaxies: individual: M 33
© ESO, 2002
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