[Previous] | [Session 35] | [Next]
J.B. Corliss (University of Wisconsin, Madison, WI), A.E. Potter (National Solar Observatory, Tucson, AZ), F. Scherb, R.C. Woodward (University of Wisconsin, Madison, WI), R.M. Killen (University of Maryland, College Park, MD)
We obtained images of the sodium emission surrounding Io at high spectral resolution (R=~150,000), using the National Solar Observatory McMath-Pierce stellar spectrograph and a 10x10 arc second image slicer. At this resolution, we can distinguish different velocity components in the sodium emission line profile. The intensity of these components varies, depending on local magnetospheric conditions at Io. In some cases, we can separate these components and generate images of each. The sodium emission was unusually bright on November 20, 1999. This, combined with excellent seeing conditions, allowed us to generate images for that night of different populations of sodium, each having distinctly different velocities. We observed the changes in these populations over a period of about three hours following emergence of Io from eclipse by Jupiter. These observations were part of our continuing observations of the increases observed in sodium emissions following emergence of Io from eclipse, and we will summarize the current status of these observations. This work was supported by the NASA Planetary Astronomy Program and the National Solar Observatory, Tucson, Arizona.
If the author provided an email address or URL for general inquiries,
it is as follows:
Bulletin of the American Astronomical Society, 34, #3< br> © 2002. The American Astronomical Soceity.