Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.4501l&link_type=abstract
American Astronomical Society, 198th AAS Meeting, #45.01; Bulletin of the American Astronomical Society, Vol. 33, p.846
Other
Scientific paper
Although O 6 is found in spectra of stars with temperature classes from O3 to B1, it is a ``superion" in the winds of those stars; i.e., it cannot be formed by the photospheric radiation field alone. It is usually thought that O 6 is produced by ensembles of shocks embedded in the wind, which might be produced by the strong line-driven instability. Therefore, the shapes and strengths of the O 6 lines are not determined by the stationary structure of the stellar wind, but by the distribution, strength, and variability of the shocks. To assess the possible origins of O 6 in the winds of such stars, we undertook a snap-shot survey of repeated observations toward Galactic and Large Magellanic Cloud stars with the Far Ultraviolet Spectroscopic Explorer (FUSE). The data consist of 2 or 3 observations spaced unequally over a variety of time scales, typically a few days to several months. The preliminary results of this survey show that the O 6 wind variability, far from being an anomaly, is a normal characteristic, as for the other unsaturated wind lines. The strengths and shapes of the variations can be very different from star to star. The FUSE bandpass allows us to observe simultaneously other ions, such as S 4, and a systematic comparison is presented between O 6 and S 4. We briefly discuss the implications that the O 6 wind variability can have on interstellar O 6 measurements. This work is based on data obtained for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by the Johns Hopkins University. Financial support to U. S. participants has been provided by NASA contract NAS5-32985.
Fullerton Alex W.
Lehner Nicholas
Massa Derck
Sembach Kenneth Russell
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