Jupiter's H-3(+) emissions viewed in corrected jovimagnetic coordinates

The distribution of H-3(+) emissions in Jupiter's polar region is interpret ed in terms of the corresponding source regions and the energetic in the ma gnetosphere by reference to corrected jovimagnetic coordinates based on the VIP4 magnetic field model of J. E. P. Connerney etal. (1998, J. Geophys. R es. 103, 11929-11939). Two sets of 3.43-mu m auroral images, acquired on Ma y 31/June 1, 1996, and on July 8/July 9, 1996, using NSFCAM at NASA IRTF, w ere analyzed. Model images were generated for observed rotation phases, and the generalized inverse methodology of T. Satoh et al. (1996, Icarus 122, 1-23) is applied to pixel-by-pixel comparison of intensities to constrain t he parameters of the emission source model. The most intense emissions are found between the 12-R-j (jovian radii) and 30-R-j ovals, representing the main auroral emissions. The System-III longitudes (lambda(III)) of peak bri ghtness in this zone, lambda(III) similar to 260 degrees in the north and s imilar to 130 degrees in the south, coincide well with those of the minimum surface field magnitudes according to the VIP4 model. Between the 8-R-j an d the 12-R-j ovals, the peak brightness occurs at lambda(III) similar to 21 5 degrees in the north and at similar to 25 degrees in the south, consisten t with the Satoh ef al. (1996) System-m anomalies. These enhancements may o riginate from the "windshield wiper" effects of drifting electrons, caused by pitch angle scattering of varying efficiency from the inner to the dista nt magnetosphere. The total power emitted from the entire auroral region by the H-3(+) ion at all re-vibrational levels is estimated as 2.1 x 10(12) W in the north, and 1.2 x 10(12) W in the south. Relative contributions from the individual zones are similar to 10% from the 6- to 8-Rj zone, similar to 20% from the 8- to 12-R-j zone, similar to 25% from the 12- to 30-R-j zo ne, and similar to 45% from the polar-cap emission, respectively. (C) 1999 Academic Press.