Modeling Jovian H_3(+) Aurorae Using NSFCAM Images

Details Modeling Jovian H_3(+) Aurorae Using NSFCAM Images Modeling Jovian H_3(+) Aurorae Using NSFCAM Images

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.2224s&link_type=abstract

American Astronomical Society, DPS meeting #28, #22.24; Bulletin of the American Astronomical Society, Vol. 28, p.1146

Computer Science

Performance

Scientific paper

Distribution of H_3(+) emissions in Jupiter's polar regions has been previously mapped using a generalized inverse analysis of infrared images, acquired with ProtoCAM at NASA's IRTF in 1992. The analysis revealed uniform emission distributed around the aurora oval, and two anomalies: one fixed to Jupiter's System-III longitude and the other fixed in local time. The former is found at lower magnetic latitudes relative to the auroral oval, while the latter is found at higher magnetic latitudes. The emission source model successfully simulated the appearance of Jupiter's aurorae, for various rotation phases, as observed with ProtoCAM (Satoh et al., Icarus 122, 1-23, 1996). We have subsequently obtained higher-resolution images in 1995 and in 1996, utilizing a new infrared camera (256x256 pixels NSFCAM) and improved thermal controls of the IRTF. We compare these improved NSFCAM images with simulated images based upon the ProtoCAM model, to evaluate the performance of our inverse method and to improve the emission source model.

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