Other
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..736b&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Other
Scientific paper
ABSTRACT Introduction The Io UV footprint is an auroral feature observed close to the feet of the field lines passing through Io on both Jovian hemispheres [1]. These light emissions are caused by the electromagnetic interaction between the satellite Io and the Jovian magnetosphere. For both the north and south poles, the Io footprint appears as a bright spot followed by a faint trailing tail and occasionally followed or preceded by secondary spots. The footprint morphology and the spots multiplicity have been found to vary with the location of Io in the plasma torus [2]. Measurements of the Io footprint dimensions In the present work, we make use of the complete dataset acquired from1997 to 2007with the Space Telescope Imaging Spectrograph (STIS) and Advanced Camera for Surveys (ACS) FUV cameras onboard the Hubble Space Telescope (HST) to study the characteristics of the IFP. Among others, we analyse short exposures extracted from STIS Time- Tag sequences to measure the footprint width and length and to estimate the impact of motional blurring on standard image. The altitude of the IFP emission has been derived from images showing the IFP above the UV limb. We find that the IFP originates at altitudes as high as 1000 km (+/- 300km), giving new constraints on the energy of the precipitating electrons. Model of the Io footprint emissions Additionally, we present a 3D model of the Io footprint emissions in the 100 to 170 nm wavelength range, consisting of the H Lyman-alpha lines and Lyman and Werner H2 bands. Comparisons between simulated images and HST images enable us to resolve some ambiguities linked to the viewing geometry and to test hypotheses on the 3D emission distribution. Finally, this model allows to measure the footprint brightness on the HST images with a better estimation of the geometric effects (e.g. limb brightening). References [1] Saur J. et al. (2004), Jupiter. The Planet, Satellites and Magnetosphere, 537-560. [2] Bonfond, B. et al. (2008), GRL, 35, L05107, doi:10.1029/2007GL032418.
Bonfond Bertrand
Gérard Jean-Claude
Grodent Denis
Gustin Jacques
Jacobsen Sven
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