Imaging H_3^+ in the ionosphere of Uranus: relocation of the magnetic pole and characterization of the aurora

Details Imaging H_3^+ in the ionosphere of Uranus: relocation of the magnetic pole and characterization of the aurora Imaging H_3^+ in the ionosphere of Uranus: relocation of the magnetic pole and characterization of the aurora

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006noao.prop..247m&link_type=abstract

NOAO Proposal ID #2006B-0247

Physics

Optics

Scientific paper

We propose using Keck II to clearly observe Uranus`s auroral structure for the first time. This will improve our understanding of the planet's ionosphere and magnetosphere. Only a basic model of Uranus's magnetosphere exists, based primarily on Voyager 2`s fly-by. The only successful post-Voyager observations pertaining to Uranus`s magnetic environment have been in the infrared. We have H_3^+ spectra that indicate solar wind control of the intensity levels. Using the NSFCam instrument on IRTF, we have detected variations in surface intensity of H_3^+ emission that show possible correlation with the Voyager auroral images, but the images are too blurred to show precise detail of the morphology; adaptive optics are necessary. Nonetheless, by quantifying the proportion of H_3^+ created by solar EUV, we determined there must be a separate auroral component. If this component can be better constrained, it will lead to a rediscovery of the magnetic pole and a more accurate determination of the rotation rate. These observations are particularly timely, as Uranus approaches equinox in 2007 and becomes the focus of the wider astronomical community.

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