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JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 101, NO. A4, PAGES 7685–7695, 1996

Hot plasma parameters of Jupiter's inner magnetosphere

B. H. Mauk

Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland


S. A. Gary

Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland


M. Kane

Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland


E. P. Keath

Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland


S. M. Krimigis

Applied Physics Laboratory, Johns Hopkins University, Laurel, Maryland


T. P. Armstrong

Department of Physics and Astronomy, University of Kansas, Lawrence


Abstract

The bulk parameters of the hot (>20 keV) plasmas of Jupiter's inner magnetosphere, including the vicinity of the Io plasma torus, are presented for the first time (L = 5 to 20 R J ). The low-energy charged particle (LECP) instrument on Voyager 1 that obtained the data presented here was severely overdriven within the inner regions of Jupiter's magnetosphere. On the basis of laboratory calibrations using a flight spare instrument, a Monte Carlo computer algorithm has been constructed that simulates the response of the LECP instrument to very high particle intensities. This algorithm has allowed for the extraction of the hot plasma parameters in the Jovian regions of interest. The hot plasma components discussed here dominate over other components with respect to such high-order moments as the plasma pressures and energy intensities. Our findings include the following items. (1) Radial pressure gradients change from positive (antiplanetward) to negative as one moves outward past about 7.3 R J . While the observed hot plasma distributions will impede the radial transport, via centrifugal interchange, of iogenic plasmas throughout the Io plasma torus regions out to 8 R J , the plasma impoundment concept of Siscoe et al. [1981] for explaining the so-called “ramp” in the flux shell content profile of iogenic plasmas (7.4–7.8 R J [Bagenal, 1994]) is not supported. (2) We predict a radial ordering for the generation of the aurora, which translates into a latitudinal structure for auroral emissions. Planetward of about 12 R J , intense aurora (10 ergs/(cm2 s) precipitation) can only be caused by ion precipitation, whereas outside of about 12 R J such intense aurora can only be caused by electron precipitation. Uncertainties concerning the causes of Jovian aurora may stem in part from failures of some observations to resolve the latitudinal structure that is anticipated here and possibly from changes in the auroral configuration and/or charged particle spectral properties since the Voyager epoch.

Received 10 October 1995; accepted 22 December 1995.

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Citation: Mauk, B. H., S. A. Gary, M. Kane, E. P. Keath, S. M. Krimigis, and T. P. Armstrong (1996), Hot plasma parameters of Jupiter's inner magnetosphere, J. Geophys. Res., 101(A4), 7685–7695.