Issue |
Astron. Astrophys. Suppl. Ser.
Volume 116, Number 2, April II 1996
|
|
---|---|---|
Page(s) | 257 - 287 | |
DOI | https://doi.org/10.1051/aas:1996113 | |
Published online | 15 April 1996 |
Long- and short-term variability in O-star winds. I. Time series of UV spectra for 10 bright O stars *,**
1
Astronomical Institute “Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2
Center for High Energy Astrophysics (CHEAF), Kruislaan 403 1098 SJ Amsterdam, The Netherlands
3
Science Programs, Computer Sciences Corporation, 10000-A Aerospace Road, Lanham-Seabrook, MD 20706, U.S.A.
Send offprint request to: L. Kaper
Received:
18
May
1995
Accepted:
27
September
1995
An atlas of time series of ultraviolet spectra is presented for 10 bright O
stars. The spectra were obtained with the International Ultraviolet
Explorer during seven observing campaigns lasting several days over a period
of 6 years. The UV P Cygni lines in 9 out of the 10 studied stars exhibit a
characteristic pattern of variability in the form of discrete absorption
components (DACs) migrating through the absorption troughs on a timescale of
a day to a week. This pattern is significantly different for each star, but
remains relatively constant during the time span of our observations for a
given star. A quantitative evaluation of the statistical significance of the
variability is given.
The winds of a number of stars appear to vary over the full range of wind
velocities: from 0 km s-1 up to velocities exceeding the terminal velocity
of the wind as measured by the asymptotic velocity reached by DACs.
The amplitude of variability reaches a maximum at about 0.75
in
the unsaturated resonance lines of stars showing DACs. In saturated
resonance lines we find distinct changes in the steep blue edge. This
edge variability is also found, although with smaller amplitude, in
unsaturated resonance lines. The subordinate line of N IV at
1718 Å in ξ Per shows weak absorption enhancements at low
velocities in the blue-shifted absorption that are clearly associated
with the DACs in the UV resonance lines.
We interpret these three manifestations of variation as reflecting a
single phenomenon. The DACs are the most conspicuous form of the
variability. The changes at the edge can often be interpreted as DACs,
but superposed on a saturated underlying wind profile; in many cases,
however, at the same time two or more absorption events in different
stages of their evolution can be identified in the unsaturated profiles,
hampering a detailed interpretation of the edge variability. The low
velocity absorption enhancements in the subordinate lines are the
precursors of DACs when they are formed close to the star.
The constancy of the pattern of variability over the years and the
(quasi-)periodic recurrence of DACs strongly suggest that rotation of
the star is an essential ingredient for controlling wind variability. The
observation of low-velocity variations in subordinate lines, which are
supposedly formed at the base of the stellar wind, indicate an origin of
wind variability close to or at the photosphere of the
star.
Key words: stars: early type / stars: mass loss / ultraviolet: stars
© European Southern Observatory (ESO), 1996