Other
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3403w&link_type=abstract
American Astronomical Society Meeting 208, #34.03; Bulletin of the American Astronomical Society, Vol. 38, p.110
Other
Scientific paper
I will summarize the results of our FUSE survey of OVI absorption in and near the Milky Way. Our original survey (May 2003) was based on 100 sightlines with S/N ratio >3. We now have almost 200 sightlines. Galactic OVI absorption at velocit ies between -100 and 100 km/s is ubiquitous, with column densities between 13.8 and 14.8. High-velocity (|v|>100 km/s) OVI absorption is also seen in many directions.The low-velocity OVI probably originates in or close to the galactic disk. It has a very patchy distribution, showing a North-South, but on average it seems to have a scale height of 2.3 kpc. The OVI kinematics show no obvious relation to galactic rotation, inflows or outflows. A comparison of OVI with CIV and NV suggests that the low-velocity highly-ionized species originate in conductive interfaces, although corrections for CIV photoionization still need to be made.The high-velocity OVI appears associated with neutral and ionized gas at larger distances. OVI is seen toward most neutral HVCs, especially complex C and the Magellanic Stream. High-velocity OVI is weak or absent toward HVC complex A. There are also many detections of high-velocity OVI (and other ions) in directions with N(HI)<2x1018 cm-2 (the detection limit of radio surveys). Photoionization modeling of other ions detected at high velocity shows that the high-velocity OV I probably also originates in interfaces between hot and cool gas. The kinematic al distribution of the high-velocity HI and OVI suggests that the HVCs are samples of a population of clouds forming an 200 kpc radius corona around the Milky Way.
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