Abstract
Abstract. We analyse the interchange or flute instability of the equatorial plasma disk in Jupiter's middle magnetosphere. Particular attention is paid to wave coupling between the dense plasma in the equatorial disk and the more rarefied plasma at higher latitudes, and between the latter plasma and the conducting ionosphere at the feet of the field lines. It is assumed that the flute perturbations are of small spatial scale in the azimuthal direction, such that a local Cartesian approximation may be employed, in which the effect of the centrifugal acceleration associated with plasma rotation is represented by an "external" force in the "radial" direction, perpendicular to the plasma flow. For such small-scale perturbations the ionosphere can also be treated as a perfect electrical conductor, and the condition is determined under which this approximation holds. We then examine the condition under which flute perturbations are at the threshold of instability, and use this to determine the corresponding limiting radial density gradient within the plasma disk. We find that when the density of the high-latitude plasma is sufficiently low compared with that of the disk, such that coupling to the ionosphere is not important, the limiting radial density profile within the disk follows that of the equatorial magnetic field strength as expected. However, as the density of the high-latitude plasma increases toward that of the equatorial disk, the limiting density profile in the disk falls increasingly steeply compared with that of the magnetic field, due to the increased stabilising effect of the ionospheric interaction. An initial examination of Galileo plasma density and magnetic field profiles, specifically for orbit G08, indicates that the latter effect is indeed operative inside radial distances of ~20 RJ. At larger distances, however, additional density smoothing effects appear to be important.
Highlights
A dominant feature of Jupiter’s middle magnetosphere is the equatorial disk of plasma produced from the atmosphere of the moon Io, which orbits deep within the equatorial magnetosphere at a radial distance of ∼6 RJ, and produces a heavy ion plasma whose overall source strength is ∼1000 kg s−1 (e.g. Hill et al, 1983; Vasyliunas, 1983; Khurana and Kivelson, 1993; Bagenal, 1997; Delamere and Bagenal, 2003)
In this paper we have examined the flute instability of the equatorial disk of iogenic plasma in Jupiter’s middle magnetosphere
Particular attention has been paid in the analysis to the wave coupling between the dense plasma in the equatorial disk and the more rarefied plasma at higher latitudes, and between the latter plasma and the conducting planetary ionosphere
Summary
A dominant feature of Jupiter’s middle magnetosphere is the equatorial disk of plasma produced from the atmosphere of the moon Io, which orbits deep within the equatorial magnetosphere at a radial distance of ∼6 RJ , and produces a heavy ion (sulphur and oxygen) plasma whose overall source strength is ∼1000 kg s−1 (e.g. Hill et al, 1983; Vasyliunas, 1983; Khurana and Kivelson, 1993; Bagenal, 1997; Delamere and Bagenal, 2003). The centrifugal action of the cool component, which contains most of the plasma mass, combined with the pressure gradient of the hot component, which contains most of the plasma thermal energy, act to stretch the magnetic field lines outward away from the planet, associated with an azimuthal current, which is a characteristic feature of the middle magnetosphere region (Acuna et al, 1983; Mauk et al, 1985; Caudal, 1986; Bunce and Cowley, 2001; Khurana, 2001) This general picture of the physics of Jupiter’s middle magnetosphere has been current for a significant period, a detailed understanding of the nature of the associated transport processes, and their relation to the plasma properties, has proven elusive. This threshold profile can be further smoothed by slower instabilities, though this aspect is not considered here
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