Other
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3701f&link_type=abstract
American Astronomical Society Meeting 208, #37.01; Bulletin of the American Astronomical Society, Vol. 38, p.112
Other
Scientific paper
One of the key discoveries of the FUSE satellite has been the detection of a network of highly ionized clouds moving at high velocities with respect to the local standard of rest. These clouds are detected through their high-velocity (100 km/s < vLSR < 400 km/s) O VI absorption lines seen in QSO spectra. I review recent absorption line studies of high-velocity O VI, mentioning distribution on the sky, kinematics, counterparts in other ions, ionization processes, and origin models. Approximately 25% of high-velocity O VI absorbers have counterparts in H I 21 cm emission, but the remaining 75%, the "highly ionized HVCs", do not. Both 21 cm-bright and highly ionized HVCs contain multiple phases of absorption, with the properties of O VI similar in both cases. The highly ionized HVCs may therefore represent the low column density tail of the HVC population, with the O VI arising at the conductive or turbulent interfaces between the H I cores and a hot (106 K) surrounding medium. Direct distance information is lacking for the highly ionized HVCs. However, both H I HVCs and hot, X-ray absorbing gas exist in the vicinity of the Milky Way. If highly ionized HVCs trace the boundary between these two phases, they must be Galactic themselves.
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