Other
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21442502d&link_type=abstract
American Astronomical Society, AAS Meeting #214, #425.02; Bulletin of the American Astronomical Society, Vol. 41, p.694
Other
Scientific paper
Using the Far Ultraviolet Spectroscopic Explorer (FUSE), we have conducted a search for O VI λ1032 emission along sight lines one arcmin from several nearby white dwarfs that have also been observed with FUSE. The white-dwarf spectra present a wide range of O VI absorption properties, ranging from no detectable O VI to strong circumstellar absorption. Of the 15 white dwarfs in our sample, three show O VI emission at three-sigma significance. Toward WD 1800+685, we have observations along three lines of sight, offset from the star by 1 to 3.5 arcmin, two of which show significant O VI emission. Along the sight line closest to the star, the velocity of the emitting gas is consistent with that of the interstellar O I, C II, and O VI features in the star's FUSE spectrum (Savage & Lehner 2006). Assuming that the same gas is responsible for both emission and absorption, we can derive its physical properties: an electron density ne = 0.2 cm-3, a pressure P/k near 105 K cm-3, and a path length through the emitting gas of 0.3 pc, parameters similar to those derived for other nearby O VI emitting regions. The star's distance (159 pc) and O I column density suggest that it lies beyond the dense neutral boundary of the Local Bubble. If so, then the O VI-bearing gas probably lies within the Local Bubble wall.
This work is supported by NASA grant NNX06AD30G.
Dixon William Van Dyke
Sankrit Ravi
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