Jupiters H+3 Emissions Viewed in Corrected Jovimagnetic Coordinates.pdfVIP

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Jupiters H+3 Emissions Viewed in Corrected Jovimagnetic Coordinates.pdf

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Jupiters H+3 Emissions Viewed in Corrected Jovimagnetic Coordinates.pdf

Icarus 141, 236–252 (1999) Article ID icar.1999.6173, available online at on Jupiter’s H+3 Emissions Viewed in Corrected Jovimagnetic Coordinates Takehiko Satoh Frontier Research Center for Computational Sciences, Science University of Tokyo, 2641 Yamazaki, Noda-shi, Chiba 278-8510, Japan E-mail: tsatoh@rs.noda.sut.ac.jp and J. E. P. Connerney Laboratory for Extraterrestrial Physics, Code 695, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771 Received December 15, 1998; revised April 26, 1999 The distribution of H3+ emissions in Jupiter’s polar region is interpreted in terms of the corresponding source regions and the energetic in the magnetosphere by reference to corrected jovimagnetic coordinates based on the VIP4 magnetic ?eld model of J. E. P. Connerney et al. (1998, J. Geophys. Res. 103, 11929–11939). Two sets of 3.43-μm auroral images, acquired on May 31/June 1, 1996, and on July 8/July 9, 1996, using NSFCAM at NASA IRTF, were 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 the parameters of the emission source model. The most intense emissions are found between the 12-Rj ( jovian radii) and 30-Rj ovals, representing the main auroral emissions. The System-III longitudes (λIII) of peak brightness in this zone, λIII ～ 260? in the north and ～130? in the south, coincide well with those of the minimum surface ?eld magnitudes according to the VIP4 model. Between the 8-Rj and the 12-Rj ovals, the peak brightness occurs at λIII ～ 215? in the north and at ～25? in the south, consistent with the Satoh et al. (1996) System-III anomalies. These enhancements may originate from the “windshield wiper” effects of drifting electrons, caused by pitch angle scattering of varying ef?ciency from the inner to the distant magnetosphere. The total power emitted from the entire auroral region by the H+3 io