Issue |
A&A
Volume 405, Number 3, July III 2003
|
|
---|---|---|
Page(s) | 1043 - 1056 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20030601 | |
Published online | 30 June 2003 |
A search for OVI in the winds of B-type stars
1
Dept. of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218, USA
2
Dept. of Physics and Astronomy, University of Victoria, PO Box 3055, Victoria, BC, V8W 3P6, Canada
3
Dept. of Astronomy, University of Wisconsin, 475 N. Charter St., Madison, WI 53706, USA
4
SGT Inc., Code 681.0, NASA's Goddard Space Flight Center, Greenbelt, MD 20771, USA
Corresponding author: J. Zsargó, jzsargo@astro.phyast.pitt.edu
Received:
29
January
2003
Accepted:
18
April
2003
We have conducted a survey of FUSE spectra of 235 Galactic B-type stars
in order to determine the boundaries in the H-R diagram for the production
of the superion in their winds.
By comparing the locations and morphology of otherwise unidentified
absorption features in the vicinity of the
resonance doublet with
the bona fide wind profiles seen in archival IUE spectra of the resonance
lines of
,
and
, we were able to detect
blueshifted
lines in the spectra of giant and supergiant
stars with temperature classes as late as B1.
No features attributable to
were detected in dwarfs later than
B0, or in stars of any luminosity class later than B1, although
our ability to recognize weak absorption features in these stars is severely
restricted by blending with photospheric and interstellar features.
We discuss evidence that the ratio of the ion fractions of
and
is substantially different in the winds of early B-type stars
than O-type stars.
Key words: stars : early-type / stars : mass-loss / ultraviolet : general
© ESO, 2003
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